First Light Science with the GTC Program and Abstracts Organizing Committees

LOC – Local Organizing Committee Chris Packham (co-Chair), University of Florida Rafael Guzman (co-Chair), University of Florida Anthony Gonzalez, University of Florida Vicki Sarajedini, University of Florida Stanley Dermott, University of Florida

SOC – Scientific Organizing Committee Rafael Guzman (Chair), UF, USA Jose Alberto Lopez, IAUNAM, Mexico Charles Telesco, UF, USA Elizabeth Lada, UF, USA Francisco Garzon, IAC, Spain Francisco Sanchez, IAC, Spain Itziar Aretxaga, INAOE, Mexico Jesus Gallego, UCM, Spain Jesus Gonzalez, IA-UNAM, Mexico Jian Ge, UF, USA Jordi Cepa, IAC, Spain Jose Franco, IA-UNAM, Mexico Jose Guichard, INAOE, Mexico Jose M. R. Espinosa, GTC project office, Spain Luis Colina. IEM-CSIC, Spain Marc Balcells, IAC, Spain Mariano Moles, IAA, Spain Marisa Garcia, GTC project office, Spain Stanley Dermott, UF, USA Steve Eikenberry, UF, USA Xavier Barcons, CSIC, Spain

First Light Science with the GTC Sponsors

First Light Science with the GTC would like to thank these organizations for their support of this meeting.

Research & Graduate Programs

First Light Science with the GTC General Information

Date: Main Conference: Wednesday, June 28 - Friday, June 30, 2006 Post Conference Workshops: Saturday, July 1 - Tuesday, July 4, 2006

Site of the Meeting: The Biltmore Hotel 1200 Anastasia Avenue Coral Gables, FL 33134 Tel: (305) 445-1926 FAX: (305) 913-3159 Web Site: http://www.biltmorehotel.com Oral Presentations: Merrick & Stoneman Douglas (simulcast) Poster Presentations: Tuttle, Flagler & Deering Lunch: Alhambra

Notice to Speakers: The speakers are requested to bring their Power Point presentation to the session room 30 minutes be- fore their sessions. A speaker-ready computer will be available for speakers to check their media prior to their presentations. Please check with the registration desk for details.

Notice to Poster Presenters: Pins will be provided and placed in the poster area. Each poster board is marked with a number refer- ring to the poster number in the program. Posters should be mounted by 8:00am on Wednesday, June 28 and removed by 6:00pm on Friday, June 30. Presenters are requested to be present at their posters during the coffee breaks.

Social Program: All registered participants and paid companions are invited. Tuesday, June 27, 2006 at 7:00pm Welcome Reception — Alhambra Terrace Thursday, June 29, 2006 at 6:00pm Alumni Night Reception — Alhambra Friday, June 30, 2006 at 7:30pm Conference Banquet & Fiesta — Country Club Ballroom

First Light Science with the GTC General Information

Registration: Registration includes admission to scientific sessions (oral and posters). It also includes morning and afternoon coffee breaks, the Welcome Reception (Tuesday evening), three complimentary lunches (Wednesday to Friday), the Alumni Night Reception (Thursday evening), and the Conference Banquet & Fiesta (Friday evening). Registrants will receive a folder containing conference materials, the abstract book and a list of regis- tered participants. . Late registrations fees: Regular — $450.00 (US) Accompanying person — $80.00 (US)

Mode of Payment: Credit Card (Visa, Master Card and American Express): Please specify card number, expiration date, and the name of the card holder. Personal Check: Must be drawn on a U.S. bank. Cash

Local Information: For more information about the Coral Gables, Florida area please visit the official travel site for the area at: http://www.citybeautiful.net/CGWeb/visitors.aspx

Internet Access Internet access will be available for all conference participants at the conference information table.

Hotel Restaurants & Hours: Palme d’Or: Tuesday - Thursday 6:0 0-10:30pm; Friday & Saturday 6:00-11:30pm 1200 Courtyard Grill: Breakfast 6:30-11:30am; Lunch 11:30am-5:00pm; Dinner 5:00-10:30pm Cascade (poolside): Lunch 11:30am-3:00pm; Light Snack Menu 3:00-5:30pm 19th Hole Sports Bar & Grill: Daily 6:30am-6:00pm

First Light Science with the GTC The Biltmore Hotel Conference Area Map

Main Hotel

~ Lunch ~ Welcome Reception ~ Alumni Night Reception

~ Simulcast Room ~ Hispanic Alumni Association Talk ~ General Session

Conference Center

~ Posters

~ Breaks

First Light Science with the GTC Coral Gables Area Map

First Light Science with the GTC Scientific Program — Agenda

SCIENTIFIC SESSIONS

Tuesday, June 27, 2006 5:00-7:00pm Check-in/Registration/Information Booth Open 7:00-9:00pm Welcome Reception — Alhambra Terrace

Wednesday, June 28, 2006 7:30am-6:30pm Check-in/Registration/Information Booth Open 8:30-9:00am Welcome – Merrick & Stoneman Douglas (simulcast) 9:00-10:30am Session I – Merrick & Stoneman Douglas (simulcast) 10:30-11:00am Coffee Break and Poster Viewing – Tuttle/Flagler/Deering/Bowman 11:00am-12:30pm Session II – Merrick & Stoneman Douglas (simulcast) 12:30-2:30pm Lunch – Alhambra 2:30-4:00pm Session III – Merrick & Stoneman Douglas (simulcast) 4:00-4:30pm Coffee Break and Poster Viewing – Tuttle/Flagler/Deering/Bowman 4:30-6:00pm Session IV – Merrick & Stoneman Douglas (simulcast)

Thursday, June 29, 2006 8:00am-6:30pm Check-in/Registration/Information Booth Open 8:30-10:20am Session V – Merrick & Stoneman Douglas (simulcast) 10:20-11:00am Coffee Break and Poster Viewing – Tuttle/Flagler/Deering/Bowman 11:00am-12:30pm Session VI – Merrick & Stoneman Douglas (simulcast) 12:30-2:30pm Lunch – Alhambra 2:30-4:30pm Session VII – Merrick 4:30-6:00pm Hispanic Alumni Association Talk – Members Only – Stoneman Douglas 6:00-8:00pm “Gran Telescopio Canarias: A Partnership for Discovery” Reception with high dignitaries from Spain, Mexico and the United States – Alhambra

First Light Science with the GTC Scientific Program — Agenda

Friday, June 30, 2006 8:00am-6:30pm Check-in/Registration/Information Booth Open 8:30-10:20am Session VIII – Merrick & Stoneman Douglas (simulcast) 10:20-11:00am Coffee Break and Poster Viewing – Tuttle/Flagler/Deering/Bowman 11:00am-12:30pm Session IX – Merrick & Stoneman Douglas (simulcast) 12:30-2:30pm Lunch – Alhambra 2:30-4:00pm Session X – Merrick & Stoneman Douglas (simulcast) 4:00-4:30pm Coffee Break and Poster Viewing – Tuttle/Flagler/Deering/Bowman 4:30-6:00pm Session XI – Merrick & Stoneman Douglas (simulcast) 6:00-6:10pm Closing Remarks – Merrick & Stoneman Douglas (simulcast) 8:30pm-Late Conference Dinner/Fiesta – Country Club Ballroom

Saturday, July 1, 2006 – Post Conference Workshops FRIDA Workshop – Alberto Lopez CANARICAM Workshop 1 – Chris Packham CANARICAM Workshop 2 – Charlie Telesco OSIRIS Workshop – Jordi Cepa

Sunday, July 2, 2006 – Post Conference Workshops EMIR Workshop – Francisco Garzon ELMER Workshop – Marisa Garcia NAHUAL Workshop – Eduardo Martin

Monday & Tuesday, July 3 & 4, 2006 – Post Conference Workshops 9:00am-6:00pm GOYA Workshop – Marc Balcells

First Light Science with the GTC Scientific Program — Oral Sessions SCIENTIFIC SESSIONS

Wednesday, June 29 8:30 - 8:40am Rafael Guzman Welcome 8:40 - 9:00am Jose Miguel Rodriguez The GTC: getting ready for First Light

SESSION I 9:00 - 9:30am Charles Telesco Invited Talk 9:30 - 9:50am Marisa Garcia Elmer performance: results of laboratory tests 9:50 - 10:10am Jordi Cepa OSIRIS assembly and integration 10:10 - 10:30am Chris Packham CanariCam: status and science prospects 10:30 - 11:00am Coffee Break and Poster Viewing

SESSION II 11:00 - 11:30am Artemio Herrero Invited Talk 11:30 - 11:50am Francisco Garzon EMIR, the GTC NIR imager spectrograph 11:50am - 12:10pm Alberto Lopez FRIDA: the science instrument for the GTC adaptive optics system 12:10 - 12:30pm Michelle Edwards CIRCE: the Canarias infrared camera experiment 12:30 - 2:30pm Lunch (Alhambra)

SESSION III 2:30 - 3:00pm Jesus Gonzalez Invited Talk 3:00 - 3:20pm Charo Villamariz How to observe with GTC 3:20 - 3:40pm Antonio Cabrera The GCS data processing kit 3:40 - 4:00pm James Hough New opportunities for polarization with CanariCam 4:00 - 4:30pm Coffee Break and Poster Viewing Scientific Program — Oral Sessions SESSION IV 4:30 - 5:00pm Jian Ge Invited Talk 5:00 - 5:20pm David Barrado The Lambda Orions star forming region: the Spitzer perspective 5:20 - 5:40pm Eduardo Martin Brown dwarf candidates ready for GTC follow-up 5:40 - 6:00pm Maria Morales A sensitive search for variability in late L dwarfs

Thursday, June 29 SESSION V 8:30 - 9:00am Elizabeth Lada Invited Talk 9:00 - 9:20am Rafael Rebolo Chemical composition of black hole and neutron star companions 9:20 - 9:40am Ata Sarajedini Local group stellar populations with the GTC 9:40 - 10:00am Antonio Marin-Franch Surface-brightness fluctuations in stellar populations 10:00 - 10:20am Reba Bandyopadhyay Determining the nature of the faint X-ray source population near GC 10:20 - 11:00am Coffee Break and Poster Viewing

SESSION VI 11:00 - 11:30am Emilio Alfaro Invited Talk 11:30 - 11:50am Peter Hammersley EMIR spectroscopic survey of the inner galaxy 11:50am - 12:10pm Jonathan C. Tan Star formation near supermassive black holes 12:10 - 12:30pm Elizabeth Tasker Building a virtual Milky Way 12:30 - 2:30pm Lunch and Poster Viewing (Alhambra)

SESSION VII 2:30 - 3:00pm Manuel Peimbert Invited Talk 3:00 - 3:20pm Rosa Gonzalez The warm interstellar gas in starbursts and AGNs Scientific Program — Oral Sessions 3:20 - 3:40pm Miriam Pena Deep spectroscopy of planetary nebulae and compact HII regions 3:40 - 4:10pm Almudena Alonso Invited Talk 4:10 - 4:30pm Tanio Diaz-Santos T-ReCS mid-infrared observations of local LIRGs

Friday, June 30 SESSION VIII 8:30 - 9:00am Meg Urry Invited Talk 9:00 - 9:20am Jorge P. Gallego 3D spectroscopy of luminous blue compact galaxies 9:20 - 9:40am Juha Reunanen VLT/SINFONI spectroscopy of nearby galaxies 9:40 - 10:00am Ana Matkovic Faber-Jackson relation for dE/ds0 galaxies 10:00 - 10:20am David Clark X-ray source environments in the dwarf starburst galaxy NGC1569 10:20 - 11:00am Coffee Break and Poster Viewing

SESSION IX 11:00 - 11:30am Stephen Eikenberry Invited Talk 11:30 - 11:50am Xavier Barcons Obscured and unobscured growth of supermassive black holes 11:50am - 12:10pm Patrick Roche Spatially-resolved mid-IR spectroscopy of nearby galaxy nuclei 12:10 - 12:30pm Nicolas Gruel Simulations of GTC/FRIDA observations of high-redshift galaxies 12:30 - 2:30pm Lunch (Alhambra) Scientific Program — Oral Sessions SESSION X 2:30 - 3:00pm David Koo Invited Talk 3:00 - 3:20pm Anthony Gonzalez Galaxy evolution during the epoch of cluster assembly 3:20 - 3:40pm Marc Balcells The formation epoch of ellipticals and red-sequence galaxies 3:40 - 4:00pm Luc Binette Large scale absorbers in the environment of high-z RGs 4:00 - 4:30pm Coffee Break and Poster Viewing

SESSION XI 4:30 - 5:00pm Roberto Terlevich Invited Talk 5:00 - 5:20pm Roser Pello Galaxies at z>7: probing galaxy formation with new NIRMOS 5:20 - 5:40pm Hsiao-Wen Chen Chemical enrichment of the IGM and ISM in the distant universe 5:40 - 6:00pm Mike Gladders Galaxy clusters, cosmology, and magellan instrumentation 6:00 - 6:10pm Stan Dermott Closing Remarks Scientific Program — Posters

SCIENTIFIC SESSIONS Poster Board # (1) Abel Bernal A high resolution scanning Fabry-Perot for OSIRIS (2) Beatriz Sanchez FRIDA management plan (3) Esperanza Carrasco Manufacturing of FRODOSPEC red arm optics and mounts (4) Francisco Cobos D. Expected OSIRIS efficiency (5) Francisco Reyes Faculty support (6) Javier Fuentes FRIDA system architecture (7) Jesus Gonzalez OSIRIS camera barrel (8) Luis J. Corral Elmer’s web pages (9) Mamadou N’Diaye Exploring high contrast resolution imaging for FRIDA (10) Marc Vallbe Mumbru The commissioning of EMIR (11) Maria Alejandra Di Cesare Alteration in hypothalamic NPY in CCK2 receptor knockout mice (12) S. Nicholas Raines FISICA: the Florida image slicer for infrared astrophysics and cosmology (13) Salvador Carlos Cuevas Cardona FRIDA optical design (14) Sergio Pascual Data reduction pipeline for EMIR, the Near-IR multi-object spectrograph for GTC (15) Amelia Bayo Dust settling: the luminosity function gap at M7-M8 (16) Ashley Expy Origin of the particles of the Zodiacal cloud (17) Audra K. Hernandez H-band spectral classification of intermediate-type stars (18) Benjamin Montesinos Metal abundances of stars with protoplanetary disks Scientific Program — Poster Presentations

(19) Bruno Ferreira Probing the structure of nearby embedded clusters (20) Curtis DeWitt Simulating the Doppler velocity precision of high resolution near infrared spectrographs (21) Cynthia Gomez Martin Low-mass stars and Brown dwarfs in NGC1333 (22) Herve Bouy VLT/VISIR mid-IR observations of Brown dwarfs, future prospects with GTC/Canaricam (23) James De Buizer New results from observations of massive star formation in th emid-infrared with the large aperture telescopes (24) Julian van Eyken New results from the multi-object Keck Exoplanet Tracker (25) Justin Crepp High-contrast imaging with the Hale 200” telescope at Palomar (26) Margaret Moerchen Self-regulation of agonist activity at the Y receptors (27) Mari Cruz Galvez High resolution spectroscopy of planet bearing stars (28) Naibi Marinas High-resolution mid-IR imaging of herbig Ae/Be stars: morphology of the circumstellar dust (29) Noah Rashking FLAMINGOS spectroscopy of low mass stars and Brown dwarfs in Orion (30) Nuria Huelamo Differential imaging adaptive optics observations of the protostar Elias 2-29 (31) Thomas J. J. Kehoe Stochastic collisional events in debris disks: what can be learned from the Zodiacal cloud? (32) David Martinez-Delgado Tracing tidal streams with GTC: testing the hierarchical formation of the Milky Way (33) Jordi Cepa The OTELO project: stellar component in the Groth field (34) Miriam Garcia Garcia VLT spectroscopy of massive stars in NGC5 (35) Norberto Castro Rodriguez VLT spectroscopy of massive stars in NGC5 (36) R. Scott Fisher Studying the wake of the galactic center source IRS8 Scientific Program — Poster Presentations (37) Susana Iglesias-Groth Searching with GTC for the carrier of the Anomalous Microwave Emission (38) Valerie Mikles First infrared spectroscopic identification of a chandra low-luminosity X-ray source in the galactic center (39) Aaron Grocholski Calcium II triplet abundances for a sample of LMC clusters (40) Eric Perlman The mid-infrared emission of M87 (41) Igor Drozdovsky The stellar structures around disk galaxies (42) Igor Drozdovsky Studying Galaxy Formation and Evolution from the Local Group galaxies (43) James Radomski High resolution mid-infrared imaging of seyfert nuclei: current results and the future with CanariCam on the GTC (44) Justin J. Schaefer Results of high-spacial resolution mid-IR imaging of NGC7172: and the discussion and application of results from the development of mid-IR data (45) Lauren Davis Galaxy cluster assembly at z~0.37 (46) Michael Barker The stellar populations of M33’s outer regions (47) Nancy A. Levenson Measuring the inhomogeneous obscuration of AGN with mid-infrared observations (48) Rachel Mason Mid-IR studies of nearby AGN at high spatial resolution (49) Stuart Young Spatially-resolved mid-infrared spectroscopy of IC 5063 (50) Alison Klesman Optical variability of infrared power law-selected galaxies & x-ray sources in the GOODS south field (51) Carlos Hoyos Stellar populations in luminous compact blue galaxies (52) Carlos Lopez Merger fraction in Groth strip (53) David Abreu Ks band-selected galaxy catalog 0

First Light Science with the GTC Invited Talk notes: The GTC: Getting ready for first Light Jose M. Rodríguez Espinosa; Pedro Alvarez Instituto de Astrofisica de Canarias The Gran Telescopio Canarias (GTC), with its 10.4m aperture, will be the largest telescope of its class once it is finished. The GTC is now being completed in the island of La Palma, Spain. Currently the main activity is finishing the fine tune of the servos of the main axes drives. The Nasmyth instrument rotators will be installed in May and by June we hope to start with the tests of the GTC control software. These tests will be lengthy, but hope- fully by the end of the summer we will be able to start installing Elmer performance: results from laboratory optics on the telescope. This will be done once we can make tests sure that the control software is performing adequately and it is García-Vargas, M.L.; Martin-Fleitas, J.M; Rodríguez-Espinosa, safe to start putting optics on the telescope. J.M.; Cabrera, A.; Kohley, R.; Hammersley, P.; Sánchez-Blanco, First light is therefore expected for November, with six primary E.; Maldonado, M; Vilela, R. mirror segments. Immediately after first light we will start com- Instituto de Astrofísica de Canarias missioning the Acquisition & Guiding Boxes (A&G), then with Elmer has been exhaustively tested at laboratory and it is ready the Commissioning Camera we will start monotonically improv- for being shipped to the ORM as soon as the GTC will be ready. ing the image quality of the optics, in an iterative process that The observing modes are: Imaging, Long Slit and Mask-multi- will lead to the quasi-simultaneous commissioning of the tele- object Spectroscopy, Slit-less multi-object spectroscopy, Fast scope optics, A&G boxes, and control software. The primary Photometry and Fast short-slit spectroscopy. The pupil elements mirror, as the commissioning progresses, will be populated with are composed by a full set of conventional broad band and nar- an increasing number of segments, so that in about six months row band filters as well as a set of prisms, grisms and VPHs, that from First Light the mirror is complete with 36 segments. In allow resolving powers of 200, 1000 and 2500 between 365 and about four months from first light we should be able to install the 1000nm. We have exhaustively tested the instrument at labora- first science instrument, and proceed with the commissioning of tory and each of the observing modes has been fully character- this instrument plus the remaining tasks of the telescopes optics. ized. Its high throughput and excellent image quality in combi- Eight months from First Light the second science instrument will nation with the GTC guarantee a powerful scientific return. This be brought to the telescope, and commissioning will proceed talk will summarize the performance results of the acceptance with the entire system, which means the telescope plus these tests for Imaging, Spectroscopy and Fast Modes. two science instruments. notes: It is planned that one year after First Light we will commence Science Operation. In my talk I will show the current status of the GTC and the plans for preparing and reaching both First Light and Science Operation. Finally, I will make a brief summary of the GTC science instruments highlighting its main features. notes:

OSIRIS assembly and integration Miguel Sánchez-Portal; Ana M. Pérez-García; Mirjana Povic; Jor- di Cepa; Emilio Alfaro; Ángel Bongiovanni; Héctor Castañeda; Jesús Gallego; Ignacio González-Serrano; J. Jesús González- González Invited Talk Instituto Astrofísica Canarias CanariCam: Mid-IR Astronomy at the Frontier OSIRIS (Optical System for Imaging and low Resolution Integrated Charles Telesco; Chris Packham Spectroscopy) is the optical Day One instrument for the GTC. OSIRIS University of Florida will cover the 365 to 1000 nm spectral range, featuring an 8.4 arcmin CanariCam, the GTC Day-One facility mid-IR camera, will be the field of view, and capabilities for direct imaging, both long slit and most sensitive mid-IR imager in the world. CanariCam, which is multiple object spectroscopy, and fast spectrophotometry. The combi- nearly completed in the lab at the University of Florida, will pro- nation of the OSIRIS wide field, tunable filters plus charge shuffling vide an extremely versatile tool to address a very broad range array detectors, will constitute the most powerful instrument for study- of challenging forefront astronomical problems. CanariCam’s ing faint emission-line sources at any redshift. The present contribu- multi-mode capabilities include direct imaging, coronagraphy, tion gives an overview of the instrument development, currently in its slit spectroscopy, and polarimetry. In this talk, after briefly de- assembly and integration phase before commissioning. scribing the status of CanariCam, I will highlight some of the key science areas for which each of its operational modes will be an especially incisive and informative probe. 20 notes: minosity suggesting that the mid-IR emission is a good tracer of the star formation rate (SFR). Analogous to the widely used relation between the SFR and total IR luminosity of Kennicutt (1998), we derive an empirical calibration of the SFR in terms of the monochromatic 24 micron luminosity that can be used for (high-z) luminous, dusty galaxies. We also investigate the 8 micron vs. Pa-alpha luminosity relation for the nuclei, individual HII regions, and integrated emission of our sample of LIRGs, and compare it with that found by Calzetti et al. (2005) for the central M51 HII knots.

CanariCam: Status and Science Prospects notes: Packham, C.; Telesco, C.M. University of Florida CanariCam is approaching acceptance testing in the laboratory at the UF. We briefly outline the capabilities and status of Canar- iCam. Possible science projects with CanariCam are illustrated through presentation of observations of AGN taken from T-ReCS and Michelle. notes:

EMIR, the GTC NIR imager spectrograph Francisco Garzón; David Abreu; Sonia Barrera; Santiago Becer- ril; Luz Marina Cairós; José J. Díaz; Ana Fragoso; Fernando Gago; Pablo López; Jesús Patrón; Jaime Pérez; José Luis Rasilla; Pablo Redondo; René Restrepo; Pablo Saavedra; Vicente Sán- chez; Fabio Tenegi; Marc Vallbé Instituto de Astrofísica de Canarias EMIR, currently entering into its fabrication and AIV phase, will be one of the first common user instruments for the GTC, the Invited Talk 10 meter telescope under construction by GRANTECAN at the Infrared and Star Formation Properties of Local Roque de los Muchachos Observatory (Canary Islands, Spain). Luminous Infrared Galaxies EMIR is being built by a Consortium of Spanish and French in- Artemio Herrero stitutes led by the IAC. EMIR is designed to realize one of the IAC central goals of 10m class telescopes, allowing observers to ob- tain spectra for large numbers of faint sources in an time-efficient Recent ISO and Spitzer cosmological surveys have shown that manner. EMIR is primarily designed to be operated as a MOS in the majority of IR-selected galaxies at z<1 are in the luminous IR the K band, but offers a wide range of observing modes, includ- galaxy (LIRG, infrared [8-1000 micron] luminosities of log L_IR= ing imaging and spectroscopy, both long slit and multiobject, in 11-11.9 Lsun) class, and that LIRGs make a significant contribu- the wavelength range 0.9 to 2.5 μm. It is equipped with two in- tion to the galaxy population at z>1. We use HST/NICMOS (1- novative subsystems: a robotic reconfigurable multislit mask and 1.9 micron continuum and Pa-alpha), Gemini/T-ReCS (8 and 10 disperssive elements formed by the combination of high quality micron), and Spitzer (8 and 24 micron) observations to study the diffraction grating and conventional prisms, both at the heart IR and star-formation properties of a representative sample of of the instrument. The present status of development, expected local (distances of 35 to 75 Mpc) LIRGs. performances, schedule and plans for scientific exploitation are described and discussed. The development and fabrication of The NICMOS and T-ReCS imaging data provide spatial reso- EMIR is funded by GRANTECAN and the Plan Nacional de As- lutions of 25-100 pc and cover the central 3.3-7.1 kpc regions tronomía y Astrofísica (National Plan for Astronomy and Astro- of these galaxies. The most IR luminous LIRGs in our sample physics, Spain). contain a sizeable population of HII regions with H-alpha lumi- nosities comparable to that of 30 Doradus, with about half of the notes: sample containing HII regions significantly brighter than those observed in normal galaxies. These luminous HII regions are also bright mid-IR emitters, as demonstrated by the impressive correspondence between the NICMOS Pa-alpha (HII emission) and the T-ReCS mid-IR (hot dust+PAH emission) morphologies. There is a linear empirical relationship between the mid-IR 24 micron and hydrogen recombination (extinction-corrected Pa-alpha) luminosity with very small scatter for our sample of moderately dust-embedded (Av ~ 2-6 mag over the Pa-alpha emitting regions) LIRGs, and HII regions in the central regions of M51. This relation holds over more than four decades in lu- 21 FRIDA: THE SCIENCE INSTRUMENT FOR THE ADAPTIVE OP- How to observe with GTC TICS SYSTEM OF GTC Charo Villamariz Alberto Lopez Grantecan S.A. UNAM I will present the details about how to proceed if you want to ob- This contribution presents the current stage of design for FRIDA, serve with GTC. Special attention will be devoted to our Phase the infrared imager and integral field spectrograph that will op- II tool, the software that will allow GTC users to produce their erate with the adaptive optics system of GTC. The capabilities of observing programmes. FRIDA will include diffraction limited imaging in broad and nar- notes: row band filters with relatively large field of views and integral field spectroscopy with resolutions R~ 1000 -- 30,000. FRIDA is a collaborative project among the main GTC partners, namely, Spain, Florida and Mexico. notes:

the GCS data processing kit Antonio Luis Cabrera Lavers; César Enrique García Dabó Grantecan S.A. As part of the GTC Control System (GCS) a data processing package is being developed. We will describe the performance of the Data Processing Kit (DPK), using real data obtained dur- CIRCE: The Canarias infrared camera experiment ing the preliminary tests made prior to the commissioning of the Edwards, M.L.; Eikenberry, S.S.; Marin-Franch, A.; Charcos- GTC (both with a Refractor and the Acquisition and Guiding Llorens, M; Rodgers, M.; Julian, J.; Raines, S.; Packham, C. Cameras). Some examples of the versatility of this pipeline will University of Florida be shown. Comparisons with Data Reduction Packages that are more commonly used (e.g., those IRAF-based) have been made We report on the design status of the Canarias InfraRed Cam- to show the DPK performance. era Experiment (CIRCE), a near-infrared visitor instrument for the 10.4-meter Gran Telescopio Canarias (GTC). Besides func- notes: tioning as a 1-2.5 micron imager, CIRCE will have the capacity for narrow-band imaging, low- and moderate- resolution grism spectroscopy, and imaging polarimetry. Other design features include fully cryogenic filter, slit, and grism wheels, high-speed photometry modes, and broad-band imaging in J, H, and Ks fil- ters. We anticipate that a myriad of scientific projects will benefit from CIRCE’s unique combination of capabilities. notes:

New opportunities for polarimetry with Canari- Cam J.H. Hough; D.K. Aitken University of Hertfordshire The combination of a 10-m class telescope and dual-beam po- larimetry promises to give very large gains in performance open- ing up many scientific opportunities. Imaging polarimetry will provide structures of magnetic fields at spatial resolutions that will not be available until ALMA and spectropolarimetry can provide detailed information on the nature of dust grains in a Invited Talk variety of environments ranging from circumstellar disks to the González, Jesús tori around AGN. Institute for Astronomy notes: To be confirmed. notes:

22 Invited Talk Brown dwarf candidates ready for GTC follow- An All Sky Extrasolar Planet Survey with New up Generation: Multiple Object Doppler Instruments Eduardo Martin Jian Ge IAC University of Florida I will present an overview of ongoing searches for brown dwarfs The All Sky Extrasolar Planet Survey is to monitor ~ 1 million in clusters, the field and star-forming regions, and I will summa- nearby bright stars (V=8-13) for detecting tens of thousands of rize what GTC can do to follow-up on them to characterize their extrasolar planets between 2006-2020 using the new genera- basic properties. tion multiple object Dispersed Fixed-delay Interferometer Dop- notes: pler instruments at the Sloan Digital Sky Survey (SDSS) 2.5-m telescope. Follow-ups with single object Doppler instruments at other telescopes can potentially increase the total number of de- tected planets by more than a factor of two. The initial results (in- cluding planet detection) from an on-going planet survey at the Kitt Peak 0.9-m Coude feed/2.1-m telescopes using a single ob- ject new generation high throughput Doppler instrument called Exoplanet Tracker will be presented. The early scientific results from the first full-scale multiple object Doppler instrument at the SDSS telescope called the W.M. Keck Exoplanet Tracker with 60 A sensitive search for variability in late l dwarfs object capability will also be presented. M. Morales-Calderon; J.R. Stauffer; J.D. Kirkpatrick; S. Carey; C.R. notes: Gelino; D. Barrado y Navascues; L.Rebull; P. Lowrance; M. Marley; D. Charbonneau; B. Patten; K.Luhman; S.T. Mageath;D.Buzasi LAEFF-INTA We have conducted a photometric monitoring program of 3 late-L brown dwarfs looking for a signal of changes in their atmo- spheres. The observations were performed using IRAC/SPITZER 4.5 μm and 8 μm bandpasses with observations that lasted for at least one rotational period of the object. One sigma rms-un- certainties of less than 3 mmag at 4.5 μm and, around 9 mmag at 8 μm. Two, out of the three objects studied exhibit some rotational The Lanbda Orionos Star Forming Region: The modulation in their light curves at 4.5 μm with periods of 7.4 Spitzer Perspective hr and 4.6 hr and peak-to-peak amplitudes of 10 mmag and 8 mmag. However, the feature is not confirmed by the 8 μm D. Barrado y Navascués; M. Morales Calderón; J.R. Stauffer data. Among the IRAC bandpasses, the shorter wavelengths LAEFF-INTA probe most deeply into late L dwarf atmospheres than the lon- The Head of Orion is a complex star forming region which in- ger wavelengths, generally above the region models predict is cludes a young open cluster (Collinder 69, about 5 Myr), two occupied by the clouds. However, there are some instrumental dark clouds (Barnard 30 and Barnard 35, with younger popula- effects that could affect the photometry at 4.5 μm and thus, we tions) and another younger areas (LDN 1588 and LDN1603). cannot confirm the variability to be real. If we assume that the We have observed one square degree in each of these regions two objects are variable, the size of the feature would be a small in order to study the stellar and substellar population. These data percentage of the visible hemisphere. If instead, the variability have been complemented with optical and near infrared pho- shown by our targets has an instrumental origin, our non-vari- tometry and spectroscopy. Among the properties we have ana- able L dwarfs could be either completely covered with clouds lyzed are the Initial Mass Function for each association, circum- or objects whose clouds are smaller and uniformly distributed stellar disks and their properties, and the fraction of members along its atmosphere. Such scenarios would lead to very small with disks, and tried to explain all these properties in the context photometric variations. of the differences in the local environment and the evolution The same technique used for the search of variability has been notes: used in optical and NIR images of the cluster Collinder 69 (~5 Myr), in the Lambda Orionis Star Forming Region, looking for signs of deuterium pulsation. The good pixel sampling of Osiris would avoid some of the instrumental effects we found in the Spitzer data and, its fast photometry mode will provide very ac- curate and well sampled light curves for these sort of searches. notes:

23 Invited Talk notes: Embedded Clsuters: Laboratories for Understan- indg Star Formation Elizabeth Lada University of Florida Results from near-infrared imaging surveys have suggested that most stars in our Galaxy form in embedded stellar clusters. Consequently, establishing the properties of young stars in such environments is essential to understanding the process of star formation, early stellar evolution and the overall likelihood of the existence of planetary systems in the Galaxy. In this talk, I will present some of the first results from our FLAMINGOS near- Surface-brightness fluctuations in stellar popu- infrared imaging and spectroscopic surveys of nearby giant mo- lations lecular clouds and discuss their implications for cluster forma- tion and evolution, the low mass IMF and circumstellar disks. Antonio Marin-Franch; Antonio Aparicio University of Florida notes: A new theoretical calibration of surface-brightness fluctuations (SBF) for single age, single metallicity stellar populations is pre- sented for the optical and near-IR broad-band filters, as well as for the HST WFPC2 and ACS filters. The IAC-star code is used. Two Padua and the Teramo stellar evolution libraries have been considered. A set of single-burst stellar populations (SSP) with a wide range of ages (3Gy-15Gy) and metallicities (Z=0.0001- 0.03) have been computed using each one of the three consid- ered stellar evolution libraries. For each SSP, color indexes and SBF magnitudes are given for the filters U, B, V, R, I, J, H, K, F218W, F336W, F439W, F450W, F555W and F814W, and for the Chemical composition of black hole and neutron first time, an uncertainty has been estimated for the SBF theo- star companions retical calibration. R. Rebolo; J. González-Hernández; G. Israelian IAC Although some differences might be addressed, the Padua and Teramo stellar evolution libraries provide comparable SBF re- Stars orbiting black holes and neutron stars offer unique op- sults. A detailed comparison of the present SBF calibrations with portunities to understand the origin of compact objects. The both previous calibrations and observational data is also pre- secondaries may have been exposed to the supernova material sented. ejected when the compact remnant was formed and current at- mospheric abundances may reveal key aspects of the formation As a conclusion, Teramo based models work better than any process and the characteristics of the progenitors. We review other calibration reproducing observational data for the near- work conducted on the chemical abundances of several second- IR wavelengths. Furthermore, the age-metallicity degeneracy is aries of Low-mass X-ray binaries in the disk and halo our Galaxy, broken for low metallicity (Z<0.0037) stellar populations. its implications and prospects to extend this research with GTC. Finally, a clear relation between the B-band SBF absolute mag- notes: nitude of a stellar population and its metallicity is found for in- termediate to old populations, so the B-band fluctuation magni- tude is proposed as a metallicity tracer. The present theoretical calibration shows that the analysis of SBF provides a very pow- erful tool in the study and characterization of unresolved stellar populations. It is also shown that the near-IR is the best choice to study SBF of unresolved stellar populations because it offers a higher resolution in age/metallicity studies of early type stellar populations, and the SBF signal of a stellar population is stronger in the near-IR. This, together with the high spatial resolution, limiting magnitude and image quality of CIRCE/GTC, makes this unique to study and characterize the age and metallicity of un- Local group stellar populations with the GTC resolved early type stellar populations. Ata Sarajedini University of Florida notes: The Gran Telescopio Canarias promises to revolutionize the study of resolved stellar populations in Local Group galaxies. The combination of superior light gathering power via its large 10.4m aperture and a state-of-the-art instrument suite will make the GTC a powerful tool in unravelling the star formation and chemical enrichment histories of nearby galaxies. I will describe research projects that focus on the Local Group’s ‘other’ spiral galaxies - M31 and M33 - and how the GTC can help improve our understanding of these systems. 24 Determining the nature of the faint X-ray source notes: population near the Reba M. Bandyopadhyay; Andrew J. Gosling; Katherine M. Blundell; Stephen S. Eikenberry; Franz E. Bauer; Michael P. Muno; James C.A. Miller-Jones; Philipp Podsiadlowski University of Florida We present first results of a multi-wavelength program to study the faint discrete X-ray source population discovered by Chan- dra in the Galactic Centre (GC). From IR imaging obtained with the VLT we identify candidate K-band counterparts to 75% of the X-ray sources in our sample. The near-IR magnitudes and colours of the majority of candidate counterparts are consistent Star formation near supermassive black holes with highly reddened stars, indicating that most of the Chandra Jonathan C. Tan sources are likely to be accreting binaries at or near the GC. University of Florida Follow-up IR spectroscopy with the VLT of a subset of the can- Supermassive black hole accretion and star formation appear to didate counterparts provides further constraints on the nature be intimately connected. I review the observational and theo- of this recently discovered population. In addition, we present retical evidence for this statement. I then discuss how observa- our discovery of highly structured small-scale (5-15”) extinction tional and theoretical work focussed on two systems, our Ga- towards the Galactic Centre. This is the finest-scale extinction lactic Center and the nucleus of M87, can help to improve our study of the Galactic Centre to date. understanding of these processes. notes: notes:

Building a virtual milky way Invited Talk Elizabeth Tasker; Greg Bryan Emilio Alfaro Columbia/University of Flori da Instituto de Astrofisica de Andalucia Numerical simulations have rapidly progressed to becoming To be confirmed. one of the most powerful accompaniments to observational as- tronomy. With them, we are able to model galaxies, planets and notes: stars at every angle and see their evolution through time. This piece of work describes the building of a virtual Milky Way galaxy using one of the latest hydrodynamics codes, Enzo. It is one of the most highly resolved simulations on a global scale and, in particular, produces a multiphase interstellar medium which, due to its complexity, it normally confined to small, non- star forming simulations. We study the formation of stars through gravitational instabilities in the galaxy disc and the effects of feedback from type II supernovae. We compare our results with observations of the star formation history, its surface density (Schmidt laws) and the star formation radial cut-off (Toomre Q parameter) in the disc. We also see a galactic fountain effect EMIR Spectroscopic survey of the inner galaxy when we add feedback which throws matter off the disc’s sur- P. Hammerley; F. Garzon; A. Cabrerea; M. Lopez- Corredoira; face before being drawn back down. . C. Gonzalez; T. Mahoney IAC notes: The latest infrared large scale surveys have opened up the struc- tures in the inner Galaxy. It is becoming increasingly clear that there is a bar but the form of the bar is still very controversial. The bulge is triaxial and this is often referred to as a bar, but there is also strong evidence for a second long bar are a distinct angle. Here we will briefly review the latest findings and show how the multi object spectroscopy of EMIR is ideal to extend this work by providing thousands of spectra along the rather than the few tens that are possible now.

25 Invited Talk pact HII regions. PN candidates have been selected as stellar ob- Manuel Peimbert jects with no detectable stellar continuum. Further VLT-FORS1 Insituto de Astronomia, multi-object spectroscopy, in the 3700-6800 A range has con- Universidad Nacional Autonoma de Mexico firmed the PN nature of several candidates. For several of them , the [OIII] 4363 line was detected, allowing thus a trustworthy To be confirmed. determination of chemical abundances. Most of the PNe appear notes: as low excitation nebulae. For about 8 HII regions, [OIII] 4363 was also detected and their chemical composition determined. A comparative analysis of the chemistry in both type of objects are being performed. A similar analysis is being carried out for PNe and HII regions in the dIrr NGC 6822. The characteristics of this galaxy make it similar to the LMC. This time, the data were acquired with the GEMINI South multi-object spectrograph. Our long term purpose is to analyze the chemical composition of the different populations in both galaxies and to study the star for- mation history and the chemical evolution of these objects so similar to the Magellanic Clouds. The warm interstellar gas in Starbursts and AGNs: notes: A clue for the Starburst-AGN connection and the evolution of galaxies Rosa M. Gonzalez Delgado; Enrique Perez; Clive Tadhunter; Montserrat Villar-Martin Instituto de Astrofisica de Andalucia Elucidating the relationship between intense star-formation and the AGN phenomenon is crucial to our understanding of the formation and evolution of galaxies and their SMBHs in the early universe. There have been many suggestions that starbursts play an important role in nearby AGNs. However, it is not known the role that starbursts play in more powerful distant AGNs. Invited Talk The warm interstellar gas is a very useful tracer of the kinemat- Infrared and Star Formation Properties of Local ics, the metallicity and the star formation rate in galaxies. Fur- Luminous Infrared Galaxies thermore, it is an excellent probe of the feedback processes tak- ing place in galaxies, in particular in AGNs and starbursts. Almudena Alonso DAMIR, IEM, CSIC This contribution shows how deep imaging taken with OSIRIS tuned at the emission lines Lyalpha, Halpha, [OIII], etc, of AGNs Recent ISO and Spitzer cosmological surveys have shown that (Seyferts, Radio Galaxies and QSOs) and starbursts will help to the majority of IR-selected galaxies at z<1 are in the luminous IR determine whether there is an ubiquitous link between star-for- galaxy (LIRG, infrared [8-1000micron] luminosities of log L_IR= mation and nuclear activity in powerful and distant AGNs. 11-11.9Lsun) class, and that LIRGs make a significant contri- bution to the galaxy population at z>1. We use HST/NICMOS notes: (1-1.9micron continuum and Pa-alpha), Gemini/T-ReCS (8 and 10micron), and Spitzer (8 and 24micron) observations to study the IR and star-formation properties of a representative sample of local (distances of 35 to 75Mpc) LIRGs. The NICMOS and T- ReCS imaging data provide spatial resolutions of 25-100pc and cover the central 3.3-7.1kpc regions of these galaxies. The most IR luminous LIRGs in our sample contain a sizeable population of HII regions with H-alpha luminosities comparable to that of 30 Doradus, with about half of the sample containing HII regions sig- nificantly brighter than those observed in normal galaxies. These luminous HII regions are also bright mid-IR emitters, as demon- strated by the impressive correspondence between the NICMOS Deep Spectroscopy of Planetary Nebulae and Com- Pa-alpha (HII emission) and the T-ReCS mid-IR (hot dust+PAH pact HII Regions in NGC 3109 and NGC 6822 emission) morphologies. There is a linear empirical relationship M. Peña; M. Richer; G. Stasinska; L. Hernandez between the mid-IR 24micron and hydrogen recombination (ex- UNAM tinction-corrected Pa-alpha) luminosity with very small scatter for our sample of moderately dust-embedded (A_V ~ 2-6mag (What a very large telescope can do for understanding chemical over the Pa-alpha emitting regions) LIRGs, and HII regions in evolution of galaxies) the central regions of M51. This relation holds over more than NGC3109, Sextans A and B, form a small group of gas-rich dwarf four decades in luminosity suggesting that the mid-IR emission is irregular galaxies just beyond the Local Group. They are metal a good tracer of the star formation rate (SFR). Analogous to the poor objects. NGC3109, in particular, seems to be similar to the widely used relation between the SFR and total IR luminosity of SMC, in luminosity, chemical composition and other character- Kennicutt (1998), we derive an empirical calibration of the SFR istics. From VLT “on ban- off band” imaging of the whole galaxy in terms of the monochromatic 24micron luminosity that can be we have detected more than 15 PN candidates and many com- used for (high-z) luminous, dusty galaxies. We also investigate 26 the 8micron vs. Pa-alpha luminosity relation for the nuclei, in- host galaxies of AGN shows their properties are indistinguish- dividual HII regions, and integrated emission of our sample of able from normal, inactive galaxies, supporting the “grand uni- LIRGs, and compare it with that found by Calzetti et al. (2005) fication” hypothesis that active accretion is a normal phase of for the central M51 HII knots. galaxy evolution. Estimates of black hole masses in AGN can be done, with varying degrees of accuracy, using broad emission notes: lines (properly calibrated), reverberation mapping, and/or mea- surements of stellar velocity dispersions in the host galaxies; ex- tending these estimates beyond the local Universe requires large telescopes. These and other key probes of AGN will be discussed and illustrated. notes:

T-RECS Mid-Infrared observations of local LIRGs T. Díaz-Santos; A. Alonso-Herrero; L. Colina; C. Packham; J. T. Radomski; C. M. Telesco CSIC We have obtained Gemini/T-ReCS mid-infrared (MIR) N-band (10.36μm) and Si-2 narrow-band (8.74μm) imaging, as well as 3d spectroscopy of luminous blue compact galax- low-resolution (R~68) spectroscopy of 3 galaxies drawn from ies a volume-limited sample of local Luminous Infrared Galaxies Jorge Pérez Gallego; Rafael Guzmán (LIRGs; 1011 < L_IR [8-1000μm] < 1012~LO). This sample has University of Florida also been observed with HST/NICMOS in both continuum light (1-1.9μm) and the Pa (lrest} = 1.876μm) emission line. The high Luminous Compact Blue Galaxies (LCBGs) are high surface spatial resolution achieved by T-ReCS (0.35’’ ~50-100, pc for brightness galaxies, bluer than a typical SBc and birghter than our sample), close to the diffraction limit, allows us to get in- 0.25L*, which are undergoing a major burst of star formation. sights into the dusty physical processes taking place in the nu- LCBGs are the closest counterpart of the numerous population clear regions of these galaxies. The MIR and Pa emissions show of starburst galaxies at intermediate and high redshift, including an almost perfect match in the structure and size of the HII re- Lyman-break galaxies at z~2. We have selected a representa- gions and nuclear emission of LIRGs. This agreement is not only tive sample of 24 LCBGs from the SDSS survey which, although qualitative but also quantitative. There exists a good correlation small, provides an excellent reference for characterizing LCBGs between the mid-IR and the extinction-corrected Pa luminosities as a class and comparison with current and future surveys of for individual regions of LIRGs. We also compare these luminosi- similar starbursts at higher redshift. We are carrying out a 3D op- ties with those of the HII regions in the central region of M51. tical spectroscopic study of this LCBG sample as part of an ambi- We use the spectroscopic features present in the T-ReCS spec- tious multiwavelenth program which goes from FUV (GALEX) troscopic range (i.e., the 11.3μm PAH emission, the 9.7μm Si to cm (VLA). 3D spectroscopy provides spatially resolved maps absorption feature, and the [SIV10.5μm emission line) to assess of kinematics, extinction, SFR and metallicity, in order to char- the importance of star-formation and deeply embedded AGN acterize their star formation history and mass assembly, and the emission in the central regions (100-200 pc) of local LIRGs. We role of mergers and supernova galactic winds. We present re- will conduct a similar study with CanariCam on the GTC for the sults from data taken at the 3.5-m telescope with PPAK in CAHA northern hemisphere LIRGs in this sample. and at the WIYN with DENSEPAK in KPNO. We use these data to simulate integrated rest-frame optical spectra of high redshift notes: starburst galaxies using the new generation of IR multi-object spectrographs, such as EMIR at the GTC. notes:

Invited Talk Observations of AGN with 8-10-m Telescopes VLT/SINFONI spectroscopy of nearby galaxies Meg Urry Juha Reunanen Yale University University of Leiden Large telescopes are essential to answering key questions in AGN We present the results of near-IR integral field spectroscopy of research. Determining the demographics of black holes requires nearby galaxies obtained with Adaptive Optics assisted SINFONI spectroscopic redshifts of faint objects, including obscured AGN, on VLT. The available data shows a complex nuclear environ- from deep surveys. Imaging and spectroscopic studies of the 27 ment with channels of cool molecular hydrogen and star form- notes: ing clusters. The velocity fields of the most prominent emission lines are significantly different from each other, indicating that the they arise from spatially separate regions. We discuss the ex- citation of emission lines, especially molecular hydrogen. notes:

Invited Talk The FLAMINGOS-2 Early Science Surveys & the GTC Stephen S. Eikenbarry University of Florida Upon commissioning on Gemini-South in late 2006, FLAMIN- Faber-Jackson relation for dE/DS0 Galaxies GOS-2 (F2) will be the most powerful wide-field near-infrared Ana Matkovic; Rafael Guzman imager and multi-object spectrograph designed for use on 8-m- University of Florida class telescopes. In order to take best advantage of the strengths We present spectroscopic observations of ~70 early-type galax- of F2 early in its life cycle, the instrument team has proposed ies in the core of the Coma cluster. Our sample includes ~40 to use 21 nights of Gemini guaranteed time in 3 surveys - the dwarf galaxies (dE/dS0) for which we measured velocity disper- FLAMINGOS-2 Early Science Surveys (F2ESS). The F2ESS will sion and line strength indices. We confirm that the Faber-Jack- encompass 3 corresponding scientific themes - the Galactic Cen- son relation holds for the luminous early-type galaxies. However, ter, extragalactic astronomy, and star formation. The extragalac- lower luminosity early-type galaxies follow a different relation: tic survey plays an important role in the planning of EMIR/GTC L a s2. We show that rotation cannot be responsible for this observations for the GOYA program, and the Galactic Center change of slope. survey is a precursor for key planned scientific observations with FRIDA/GTCAO. I will review the status of F2, the F2ESS surveys, Through diagnostic diagrams we examine index--velocity disper- and their impact on GTC science. sion relations which we are able to extend all the way to log s ~ 30 km/s. We also derive ages, metallicities and [a/Fe] ratios for notes: this sample of galaxies. We find follow-up studies with ELMER and/or OSIRIS on GTC of particular interest as these instruments would be able to provide observations of the Ca II triplet line for these galaxies. notes:

Obscured and unobscured growth of supermas- sive black holes X. Barcons; F.J. Carrera CSIC-UC The supermassive black holes that are seen to reside in virtu- X-ray source environments in the dwarf starburst ally the centres of all galaxies in the local Universe have most galaxy ngc1569 likely formed from small seeds (~10, MO) at high redshift (z>10). D.M. Clark; S.S. Eikenberry; S.N. Raines Although mergers and tidal capture of stars can also be ingredi- University of Florida ents, most of the growth from those seeds to the masses that we see today (millions to billions of MO) has occurred via accretion. We use deep J and Ks observations of the dwarf starburst gal- X-rays are copiously produced through all accretion phases and axy NGC1569 acquired with FLAMINGOS on the KPNO-4m therefore X-ray observations are the key tracers of the growth of together with Chandra X-ray coordinates to make an IR/X-ray these black holes. X-ray surveys conducted with Chandra and astrometric frame-tie. Once this frame-tie is in place we search XMM-Newton (and with XEUS and Con-X in the future) reveal for IR cluster counterparts to X-ray sources. Measuring J and Ks that an important fraction of the accretion occurs in obscured photometry on all clusters in NGC1569, we investigate the pho- objects - type 2 Seyferts and type 2 QSOs, besides in the classical tometric properties of the IR counterparts by comparing clusters type 1 Seyfert and QSO unobscured sources. with X-ray sources to the general population. Our analysis in- cludes a comparison with results found in a similar study per- In this presentation I will report on the current status of the formed on the Antennae galaxies (NGC4038/9). XMM-Newton Medium sensitivity Survey (XMS), where we have identified the sources responsible for about the brightest half of the accretion history in the Universe, as reflected in the Cosmic 28 X-ray Background. The sample outnumbers, in some cases by a notes: large amount, previous surveys with this or other instruments. Unobscured objects (type 1 AGN) still dominate at these flux- es, but an increasingly large fraction of obscured (type 2 AGN) sources appear at fainter fluxes. The X-ray to Optical flux ratio FX/

Fopt appears to be a good (but not perfect) discriminant between obscured (large FX/Fopt) and unobscured (small FX/Fopt) objects. Indeed, identifying spectroscopically obscured objects, even at intermediate X-ray fluxes, requires 8-10m class telescopes. FX/Fopt The tendency of X-ray sources becoming redder at fainter fluxes, means that efficient infrared multi-object spectroscopy (as will be provided by EMIR on GTC) will provide a major leap forward Invited Talk in the characterisation of the fainter half of the accretion history. David Koo Some prospects for this will be discussed. UCO/Lick Observatory, University of California notes: To be confirmed. notes:

Spatially-resolved mid-ir specroscopy of nearby galaxy nuclei Galaxy Evolution During the Epoch of Cluster As- Patrick Roche sembly Oxford University Anthony Gonzalez; S. Adam Stanford; M. Brodwin; P. R. Eisen- High spatial resolution observations of a small sample of nearby hardt galaxies with heavily obscured nuclei have been obtained with University of Florida TReCS on Gemini-South. Extended emission is detected in sev- eral of the galaxies with variations in the ionisation state of the The redshift regime z=1-2 is a critical period in galaxy evolu- gas and the column of cool dust grains on sub-arcsecond scales tion that provides key insight into both the star formation and revealed by N-band spectroscopy. The results will be discussed in mass assembly histories of the universe. While there has been terms of the distribution and properties of circumnuclear dust. dramatic recent progress in studies of field galaxies at this epoch, study of cluster galaxies has been limited due to a lack of known notes: galaxy clusters at this epoch. In this talk I will present the latest results from an extensive multiwavelength program that aims to study cluster galaxy evolution at this epoch. Using the combina- tion of photometric redshifts and a new wavelet detection algo- rithm, we have generated the first statistical, well-defined sample of galaxy clusters extending to z~1.5. Our sample includes the highest redshift cluster in the literature and more spectroscopi- cally confirmed galaxy clusters at z>1 than any other catalog. These clusters provide the redshift baseline necessary to observe build-up of the red sequence, quantify the assembly history of massive cluster galaxies, and measure evolution of the star for- Stimulations of gtc-frida observations of high- mation rate in the cluster environment. Towards these ends, we redshift galaxies are currently the panchromatic data available for the full survey Nicolas Gruel region with deep HST and Spitzer observations. Details of both University of Florida the survey and follow-up effort will be presented. Some of the most exciting new instruments currently being built notes: for the 10-meters class telescopes are near-infrared (NIR) Inte- gral Field Units (IFU) with Adapative Optics (AO), such as FRI- DA at the GTC. These NIR-IFUs will allow us to measure spatially resolved star formation maps, velocity maps, extinction maps and metallicity maps of starburst galaxies at high redshifts. These maps will provide the essential data to determine empirically the physics and timeline of galaxy assembly. Detailed simulations are needed to accurately transform the observed maps into the actual physical properties of the high redshift galaxy population. Here we present the results of very realistic simulations of obser- vations of starburst galaxies at various redshifts using FRIDA at the GTC and IRMOS at the TMT. 29 The formation epoch for elliptials and other time. Alternatively, one can use the “fossil” model, analyzing the red-sequence galaxies z ~ 0 universe as seen by SDSS and, from the numbers of stars of Marc Balcells different ages and metallicities, extrapolate back to earlier times. IAC Interestingly, both methods agree fairly well. A recent addition is the issue of the “downsizing” evolution of galaxies, were most The talk will present recent progress of the GOYA group in con- massive galaxies evolve faster and on average are older than straining the formation epoch of elliptical galaxies based on opti- lower mass ones. I will present the results of a recent investiga- cal-NIR imaging. tion that using the “fossil” method on the SDSS spectral data Further progress about the formation epoch for early-type galax- extends the Mass vs Age relation to the lowest mass galaxies. We ies rests on being able to map the continuum of z=1-2 galaxies. have also found that the older galaxies and more massive galax- I will discuss the feasibility of such measurements and various ies tend to be the most metal rich ones. possible strategies with GTC. notes: notes:

Galaxies at z>7: Probing galaxy formation with Large Scale absorbers in the environment of new NIRMOS high-z rgs R. Pello; J. Richard; D. Schaerer; J.F. Le Borgne; J.P. Kneib Luc Binette; Erika Benitez; Montserrat Villar-Martín; Jose Anto- Observatoire Midi-Pyrenees nio de Diego; Sinhue Haro Corzo We first present the results obtained from our deep survey of UNAM lensing clusters aimed at constraining the abundance of star- High Redshift Radio Galaxies (HZRGs) are the progenitors of forming galaxies at z~6-11, taking benefit from lensing magnifi- massive central cluster galaxies. Their study can provide impor- cation to improve the search efficiency and subsequent spectro- tant insights into the early formation of the most massive bound scopic studies. Deep near-IR photometry of two lensing clusters structures. Our group is particularly interested in the environ- was obtained with ISAAC/VLT. These images, combined with ment of HZRGs. Large scale absorbers have been found by Rott- existing data in the optical bands, including HST images, were gering and collaborators. These can be assimilated to enormous used to select very high redshift candidates at z>7 among the gas sheets that extend over tens of kiloparsecs. We recently optical-dropouts. Photometric selection criteria have been de- submitted a paper that ascertain the ionization state of some of fined based on the well proven dropout technique, specifically these sheets and their mass range. We studied the possibility that tuned to target star-forming galaxies in this redshift domain. The ionizing radiation from massive stars that leaked into the IGM corresponding UV Luminosity Function (LF) and SFR density might be at the origin of the ionization of the absorbers. We in- derived from these candidates seem compatible with the usual tend to observe these absorbers in more details using OSIRIS to values derived at z~5-6, but higher than the estimates obtained map their HI distribution. in the NICMOS Ultra Deep Field (UDF), in particular towards the bright end of the LF. We discuss the implications of these notes: results, as compared to model expectations, in terms of survey efficiency both in lensing and blank fields. We also summarize the present state of our ongoing spectroscopic survey in lensing fields, and the benefit expected with the new generation of NIR multi-object spectrographs (e.g. EMIR/GTC). notes:

Invited Talk Downsizing in the lowest mass galaxies Roberto Terlevich; Jesus Lopez; Elena Terlevich INAOE The cosmic history of star-formation can be studied in more than one way. Directly, using the universe as a time-machine one ob- tains the “Madau-Lilly Diagram” by direct observation and anal- ysis of the integrated SFR as a function of distance or look-back 30 Chemical Enrichment of the IGM/ISM in the Distant Universe Hsiao-Wen Chen University of Chicago I will discuss the prospect of study the chemical content of the in- tergalactic and interstellar media at high redshift using afterglow echelle spectroscopy. Specifically, I will present a comprehen- sive analysis of the circumstellar medium around GRB050730 and GRB051111, based on metal absorption features identified in exquisite echelle spectra of optical afterglows. I will discuss constraints that can be made for the burst engine, as well as for the mass loss and chemical feedback during the final evolution stages of massive stars. notes:

Galaxy clusters, cosmology, and magellan in- strumentation Mike Gladders University of Chicago / Carnegie Observatories The measurement of the cluster mass function with redshift, N(M,z), has been touted as one of a handful of promising meth- ods for measuring dark energy and its evolution with redshift. Unlike other methods, the use of clusters to study cosmology is intimately linked to our understanding of the growth of structure over cosmic time. This intimate linking of observables to baryon- ic physics makes the study of clusters both challenging and po- tentially informative. To meet this challenge we have designed several new instruments for the Magellan 6.5m Telescopes. The first, LDSS-3, is now in operation, and is the highest throughput multi-object spectrograph yet built. The second, the Gladders Image Slicing Multi-Slit Option for IMACS (GISMO), is being built now and will deploy in the latter half of 2006. GISMO, and addition to the wide-field IMACS spectrograph, allows for an order-of-magnitude increase in spatial sampling over a smallish (ACS-sized) field-of-view with excellent throughput, and unique- ly straddles the observational regime between standard multi- object spectrographs and IFUs. I will describe both instruments, and highlight their applications to galaxy cluster cosmology with several example observations drawn from the Red-Sequence Cluster Survey projects. notes:

31

Abstracts Poster (P) Presentations

First Light Science with the GTC P1 We present the design of the collimator and camera barrels that A high resolution scanning Fabry-Perot for minimize thermal effects due to the difference in the thermal OSIRIS expansion coefficient of the N-FK51 and KzFSN4 materials used in the optical design of the individual components. We include Abel Bernal; Margarita Rosado; Luis A. Martinez the tests carried out to verify the optical performance of the col- Instituto de Astronomia UNAM limator and camera as independent units. Following the directives of the interferometric mode of OSIRIS, Notes: the Mexican team has got support to acquire a scanning Fabry- Perot for Osiris. In this talk we will try to define which Fabry-Pe- rot will be selected as well as which filters need to be acquired. We will also discuss about the acquisition software. Notes:

P4 Expected OSIRIS Efficiency Francisco J. Cobos D.1; J. Jesús González G.1; José Luís Rasilla P.2 1Instituto de Astronomía, UNAM; 2Instituto de Astrofísica de Ca- narias P2 OSIRIS, the main optical (0.36-1.0 µm) 1st generation instrument FRIDA Management Plan for GTC is now in the final stages of the assembling process. All B. Sánchez; V. Bringas; S. Cuevas; J. J. Díaz; S. Eikenberry; C. main optical components of OSIRIS are finished and are being Espejo; R. Flores; F. J. Fuentes; J. Gallego; F. Garzón; P. Ham- characterized. This work summarizes the current estimation of mersley; J.A. López; R. Pello; A. Prieto; A. Watson the OSIRIS efficiency (throughput), basically a combination of IA-UNAM empirical and expected data, prior to its actual commissioning characterization. This analysis is here presented to aid the GTC FRIDA (inFRrared Imager and Dissector for the Adaptive op- Astronomical Community in the preparation of science pro- tics system of the Gran Telescopio Canarias) is being designed grams, and to maintain the current OSIRIS exposure-time cal- as a diffraction limited instrument with broad and narrow band culator up to date. imaging and integral field spectroscopy capabilities to operate in the wavelength range 0.9 – 2.5 µm. FRIDA is a collaborative Notes: project between the main GTC partners, namely, Spain, México and Florida. The main aspects for the organization and de man- agement plan of this complex instrument are described in this contribution. Notes:

P5 instrument Support Francisco Reyes University of Florida Instrument testing at the University of Florida. P3 Notes: Manufacturing of FRODOSPEC red arm optics and mounts Esperanza Carrasco1; Rosalia Langarica2; Carlos Perez; Gonzalo Paez3 1INAOE; 2IAUNAM; 3CIO FRODOSpec is a multi-purpose integral field input spectrograph for the 2m robotic Liverpool telescope, located at the Observa- torio del Roque de Los Muchachos. FRODOSpec is a collab- orative project between Liverpool John Moores University and the University of Southampton. The manufacturing of the optics and lens mounts was assigned to INAOE. Here we describe the manufacturing and testing of the spectrograph red arm optics.

34 P6 Notes: FRIDA System Architecture F.J. Fuentes; V. Bringas; S. Cuevas; C. Espejo; R. Flores; A. López; B. Sánchez; A. Watson Instituto de Astronomía – Universidad Nacional Autónoma de México FRIDA will be a common-user near infrared imager and integral field spectrograph covering the wavelength range from 0.9 to 2.5 microns. FRIDA will be installed at the Nasmyth A platform behind the GTCAO system. It will use diffraction-limited optics to avoid de- P8 grading the high Strehl ratios delivered by the GTCAO system in Elmer’s web pages the near infrared. Corral, L.J.; García-Vargas, M The status of the FRIDA system design is presented. It describes Grantecan, S.A. the breakdown of the instrument into well defined and manage- The web pages that will give the information of Elmer, the ‘emer- able subsystems and the procedures to ensure the traceability of gency’ instrument of GTC, are presented. The instrument’s char- high level requirements into subsystem specifications, in a way acteristics and throughput measures are based on the last instru- that the whole instrument will comply with the required perfor- ment tests. Also the spectroscopic time calculator tool (ETC) is mance when it is finally assembled. presented. A general description of the FRIDA layout is also presented, as Notes: well as the instrument proposed configurations for the required operation modes. General procedures are defined to perform the instrument engi- neering at system level. Notes:

P9 Exploring high contrast resolution imaging for FRIDA Mamadou N’Diaye Instituto de Astronomia UNAM We explore the possibility of introducing coronography with its P7 elements in the optical scheme of FRIDA. Coronography aims OSIRIS Camera Barrel at achieving a cancellation of a brilliant star to observe a faint object near to it. Here, the idea is to place a coronograph mask Cobos, Francisco; Espejo, Carlos; Farah, Alejandro; Fuentes, (Roddier phase mask or Lyot opaque mask) and a Gaussian apo- Javier; González, Jesús; Ruiz, Élfego; Sánchez, Beatriz; Tejada, dization mask in the FRIDA’s planes, and find the best configu- Carlos ration that would permit us to achieve the best coronographic Institute for Astronomy results. The study is done for two types of entrance pupil, hex- The Camera Barrel in the OSIRIS imager/spectrograph for the agonal or circular, in a monochromatic case, and without at- Gran Telescopio Canarias (GTC), is described in this article. The mospheric turbulences. We will see that with a good choice of barrel design has been designed and tested by the Instituto de configuration, we can achieve a diminution of the light star of a Astronomía of the University of Mexico (IAUNAM), in collabora- factor one million. tion with the Instituto de Astrofísica de Canarias (IAC), Spain. Notes: The Camera Barrel includes a set of nine lenses (three doublets and three singlets), with their respective supports and cells, as well as two subsystems: the Focusing Unit, which is a mechanism that modifies the first doublet relative position; and the Passive Displacement Unit (PDU), which uses the third doublet to main- tain the camera focal length and image quality when the ambi- ent temperature changes. This article includes a brief description of the camera barrel; de- scribes the design criteria related with performance justification; summarizes the specifications related with misalignment errors and generated stresses; and the final results of the assembly, in- tegration and verification of the camera.

35 P10 P12 The Commissioning of EMIR FISICA: The Florida Image Slicer for Infrared As- Marc Vallbe; Luzma Cairos; Paco Garzon trophysics and Cosmology Instituto Astrofisico Canarias S. N. Raines; S. S. Eikenberry; R. Guzman; N. Gruel; J. Julian; G. Boreman; J. Hoffman; M. Rodgers; P. Glenn; G. Hull-Allen; B. Overview of the processes and stages for commissioning EMIR Myrick; S. Flint; L. Comstock on the GTC. University of Florida Notes: We report on the design, manufacture, and scientific perfor- mance of the Florida Image Slicer for Infrared Astrophysics and Cosmology (FISICA) - a fully cryogenic all-reflective image slic- ing integral field unit for the FLAMINGOS near-infrared spec- trograph. Originally conceived as a bench-top demonstration proof-of-concept instrument, after three productive engineering runs at the KPNO 4-m telescope (as of 15 Oct 2005) we find that FISICA is capable of delivering excellent scientific results. It now operates as a ‘turnkey’ instrument at the KPNO 4-m tele- scope. FISICA is now open for community access as a visitor instrument on the KPNO 4-m telescope via collaboration with the instrument team, who can assist with the proposal prepa- P11 ration and observations, as well as provide the data reduction GTC photometric calibration tools for integral field spectroscopy. We review the optical and opto-mechanical design, fabrication, laboratory test results, and Di Césare M.A.; Hammersley P.L.; Rodriguez Espinosa J.M. on-telescope performance for FISICA. Instituto De Astrofisica De Canarias Designed to accept input beams near f/15, FISICA with FLAMIN- Two years ago we proposed a GTC calibration plan based on GOS slices a 16x33 arcsec field of view into 22 parallel elements techniques similar to the ones used for space telescopes cali- using three sets of monolithic powered mirror arrays, each with bration. At that time, we explained how important is to have a 22 mirrored surfaces cut into a single piece of aluminum. How- catalogue with calibration fields suitable for this telescope. We ever, slight vignetting for some field positions limits the effective showed the calibration strategy for GTC and their scientific in- field of view to 15x32 arcsec. The effective spatial sampling of struments (OSIRIS, ELMER, EMIR, FRIDA and ADQ. and GUID- 0.70 arcsec delivers 960 spatial resolution elements. Combined ING BOXES) between 0.3 and 2.7 microns. with the FLAMINGOS spectrograph, R~1300 spectroscopy over One of the most important things is to work with high precision the 1-2.4 micron wavelength range is possible, in either the J+H because these objects are candidates to standard stars. combined bandpass or the H+K combined bandpass. For that reason, we need to calculate star magnitudes with an FISICA was funded by the UCF-UF Space Research Initiative; error less than 0.01. It will be reached with an enought number FLAMINGOS was designed and was constructed by the IR In- of observations. strumentation Group (PI: R. Elston) at the University of Florida, Department of Astronomy, with support from NSF grant AST97- After 120 observation nights in both visible and near-infrared 31180 and Kitt Peak National Observatory. wavelengths, we will show the progress in the analysis of the data and the preparation of the catalogue. Although these fields Notes: will have to continue being observed we have began with the construction of stellar spectral patterns. This method gives the possibility to find the complete spectrum of the objects. In this work we will present the selected fields, photometry and spectroscopy of their stars and the beginning of the spectral pat- terns construction. Notes:

P13 FRIDA OPTICAL DESIGN S. Cuevas; S.S. Eikenberry; J.A. López; B. Sánchez; A. Watson; J. Fuentes; C. Espejo; V. Bringas; R. Flores-Meza; J.J. Díaz; F. Garzón; P.L. Hammersley; J.M. Montoya; A. Prieto; R. Toral; R. Estrada Instituto de Astronomia UNAM FRIDA performs as an Imager and a Spectrograph with an In- tegral Field Unit (IFU) on the same detector. The optical quality of the instrument shall be diffraction limited to exploit the cor- rected image provided by the GTC Adaptive Optics System (GT- CAO). In this presentation it is described the preliminary optical 36 design of FRIDA, including the Integral Field Unit. An analysis of Notes: the design performance is presented to demonstrate the compli- ance of the optical design with the input science requirements. Remark to the SOC: Please place this talk after the Alberto Lopez talk about the Science with FRIDA and before the Javier Fuen- tes talk about the architecture of FRIDA. Notes:

P16 Origin of the Particles of the Zodiacal Cloud Ashley Espy; Stan Dermott; Tom Kehoe University of Florida How do planets affect a debris disk and, conversely, how does P14 a debris disk affect the planets within it? These are questions we Data Reduction Pipeline for EMIR, the Near-IR Multi- can begin to answer by studying the zodiacal cloud; the debris Object Spectrograph for GTC disk around our own Sun. The zodiacal cloud consists of a broad low-frequency background with superimposed high-frequency S. Pascual; J. Gallego; N. Cardiel; J. Zamorano; F. J. Gorgas; C. dust bands (Low et al., 1984), which result from specific asteroid E. Garcia-Dabo;A. Gil de Paz disruptions (Dermott et al., 1985, Nesvorny et al., 2003). The Universidad Complutense de Madrid background cloud has several asymmetries, including a warp, tilt and offset from the Sun, which result from planetary pertur- EMIR is a near-infrared wide-field camera and multi-object spec- bations. These asymmetries have also been seen in the observa- trograph being built for the GTC. The Data Reduction Pipeline, tional signatures of debris disks around other stars. One of the which is being designed and built by the EMIR Universidad main outstanding questions about the zodiacal cloud is what are Complutense de Madrid group, will be optimized for handling the relative contributions of cometary and asteroidal particles. and reducing near-infrared data acquired with EMIR. Both re- The key to unlocking the source of the cloud is the dust bands, duced data and associated error frames will be delivered to the since they are known to be asteroidal and associated with spe- end-users as a final product. cific asteroid families, in particular the young families, Veritas Notes: and Karin, which represent a relatively recent injection of dust to the cloud. Using the orbits of the dust band particles created in the breakup of an asteroid family, we can model the dust bands and determine the cross sectional area of material in the bands. By considering the dynamical and collisional evolution of these dust band particles, we will extend the model to consider the zodiacal cloud as a whole and investigate whether the dust band sources also dominate the background cloud. This model will be constrained by matching the asymmetries, via the shape and amplitude of the line of sight flux profiles of the model to the data from IRAS, COBE, MSX and Spitzer. If we can model the zodia- cal cloud, its dust bands, and its asymmetries using only the dust particle orbits created in the disruption of asteroid families, we P15 will have a strong case for the cloud being largely asteroidal in Dust settling: the luminosity function gap at M7- nature. Knowing the source of the particles in the zodiacal cloud M8 also has implications to debris disks around other stars and how A. Bayo; D. Barrado y Navascués; F. Allard they formed. INTA Notes: Dobbie et al. (2002) have found evidence for an apparent gap

in the Luminosity Function at about M7-M8 spectral types (Teff ~2500 K). They suggested that this may be due to a drop in the mass-luminosity relationship caused by the onset of dust forma- tion in the atmosphere. We are investigating this issue by obtain- ing low- and medium-resolution IR spectra of M dwarfs at differ- ent ages (in ChaI, ~1 Myr; in L Orionis, ~5 Myr; in TW Hydrae Association, ~10 Myr; and in the field, a few Gyr). Our goal is

threefold:(i) to establish the Teff when the dust starts to appear in the atmosphere, by comparing spectra within the same age,(ii) to disentangle the effect of gravity on the dust formation and settling, by comparing samples of different ages,(iii) to get spec- trophotometry for a wide sample of M dwarfs (M1 to L0) to test theoretical models. Here, we report on the status of our work. 37 P17 P19 H-Band Spectral Classification of Intermediate- Probing the Structure of Nearby Embedded Clus- Type Stars ters Audra K. Hernandez; Elizabeth Lada Bruno Ferreira; Elizabeth Lada University of Florida University of Florida, We present the first results of SYIC-ITS, a classification routine We determine the stellar structure, the size, and other funda- for A0-K7 type stars via prominent H-Band equivalent widths. mental cluster parameters for a catalog of 42 nearby embedded SYIC-ITS was designed using optically known standards which clusters. are part of the large scale Near-Infrared Spectroscopic FLAMIN- By studying this large sample in a systematic way we seek to un- GOS Survey to study the evolution and formation of stars within derstand stars at the earliest stage of star formation. We find and giant molecular clouds (GMCs). Using data from the KPNO 2.1m present the results - that several cluster parameters are tightly and 4m telescopes, we attempt to derive ages for three clusters correlated with each other. These correlations give us important in the Orion Complex; NGC 2024, NGC 2071, and NGC 2068. insights into the formation and evolution of stellar systems. Our study accounts for ~65 stars with masses ranging from ~0.5-3.5 solar masses. To do this we combine these spectral Notes: types with JHK photometry, place them on the H-R diagram, and use pre-evolutionary models to derive ages. These ages are then compared with cluster ages found in an independent man- ner. If successful, this routine will aid in classify young star clus- ters unattainable in the optical due to being embedded in dusty GMCs. Notes:

P20 Simulating the Doppler Velocity Precision of High Resolution Near Infrared Spectrographs Curtis DeWitt; Jian Ge; Suvrath Mahadevan University of Florida Radial velocity searches for planets around low mass stars (SpT P18 > M3) can potentially lead to the discovery of planets with a Metal abundances of stars with protoplanetary few earth masses in the habitable zone. Since these stars are disks. optically dim, only a few hundred are available to current high Benjamin Montesinos1; Carlos Eiroa2; Alcione Mora1 resolution spectrographs. It seems obvious to attempt the search 1Instituto de Astrof; 2Universidad Autónoma de Madrid, Spain in the near infrared, where their SED’s peak. However, there are several obstacles to attaining good precision in the near infra- The analysis of circumstellar disks and their evolution requires red, the most daunting of which is the treatment dense telluric the knowledge of the ages -and other stellar parameters- of the absorption and emission, which will contaminate and shift the associated stars. The determination of the stellar age is highly line centers of the stellar spectra. We present a study of the at- dependent on the metallicity, as we have previously proved tainable precision that high resolution infrared spectroscopy will (Merín et al. 2004). We present here results of an ongoing study provide and compare several methods of calibrating out the sky of a sample of Herbig Ae/Be and Vega stars surrounded by disks. spectrum, while preserving the doppler information of the star High resolution (R~ 50000) spectra are compared with synthetic spectrum. Kurucz models to determine the metal abundances. In addition to these results, we describe the problems one faces when at- Notes: tempting to determine metal abundances in this kind of stars and how GTC will contribute to our knowledge of PMS stars with protoplanetary disks. Merín, B., Montesinos, B., Eiroa, C. and EXPORT collaboration, 2004, A&A 419, 301 Notes:

38 P21 These observations correlate well with other larger-scale outflow Low-Mass Stars and Brown Dwarfs in NGC1333 indicators and their geometries, such as what is seen in shock- excited H2 and CO emission. Cynthia Gomez Martin; Elizabeth A. Lada; Aaron Steinhauer; Joanna Levine In some cases these mid-infrared observations identify the local University of Florida maser emission as outflow or jet related. Thanks to the increase of facility-class mid-infrared imagers on large aperture telescopes We present results from a near-infrared spectroscopic study of (8-10m), we are achieving high resolutions in the mid-infrared candidate brown dwarfs and low mass stars in the young cluster (~0.25-0.60”) that allow us to see the detailed morphologies of NGC1333. Using FLAMINGOS on the KPNO 4m telescope, we the mid-infrared outflows around these young stellar sources. have obtained spectra of ~ 170 new members of the cluster and The mid-infrared emission seen from these sources is interpreted classified them via the prominent J and H band magnesium, and as arising from the directly heated dust on the walls of the out- water absorption features. The spectral types we derive range flow cavity. Such a cavity is created by the molecular outflow or between ~M1 to M9.5 with typical classification errors of 0.5-1 jet punching a hole in the dense clump of obscuring material subclasses. Combining these spectral types with JHK photom- surrounding the young stellar source. Such observations are im- etry, we are able to place the objects on the H-R diagram and portant because outflows from massive stars may demonstrate use theoretical pre-main sequence evolutionary models to de- that they form by accretion processes similar to low mass stars. termine their masses and ages. Notes: Notes:

P24 P22 New Results from the Multi-Object Keck Exoplanet VLT/VISIR mid-IR observations of Brown dwarfs, fu- Tracker ture prospects with GTC/Canaricam Julian van Eyken1; Jian Ge1; Xiaoke Wan1; Bo Zhao1; Abishek H. Bouy; E.L. Martin; N. Huelamo; G. Basri Hariharan1; Suvrath Mahadevan1; Curtis DeWitt1; Pengcheng Instituto Astrofísica Canarias; UC Berkeley Guo1; Roger Cohen1; Scott W. Fleming1; D. McDavitt1; Justin We present the results of our mid-IR observations of young brown Crepp1; French Leger2; Kaike Pan2 dwarfs in the Upper Scorpius association. We obtain mid-IR im- 1University of Florida; 2APO ages of 10 brown dwarfs with VISIR at the VLT. Six objects are The Keck Exoplanet Tracker is a precision Doppler radial veloc- detected at relatively low levels (2 to 10 sigmas). Among these, ity instrument based on a new technique which allows for multi- 4 have been resolved as multiple systems with complementary object observing for the first time. Currently being installed at adaptive optics images in the near-IR, but are not resolved in the the 2.5m Sloan telescope at Apache Point Observatory, the com- VISIR images. We discuss the frequency of disks among USco bination of Michelson interferometer and medium resolution BD and compare it to the frequency of accretors, and discuss spectrograph allows for simultaneous Doppler measurements of this study and the future prospects in the context of the future up to 56 targets, while maintaining high instrument throughput. GTC/Canaricam instrument and its greater sensitivity. Using a single-object prototype of the instrument at the KPNO Notes: 2.1m telescope, we previously discovered a 0.49 MJup planet, HD 102195b (ET-1), orbiting with a 4.11 period. Other promising candidates are also being followed up. During recent first light observations with the Keck Exoplanet Tracker we were able to successfully obtain 56 simul- taneous fringing stellar spectra on several different fields, of a quality sufficient to begin a survey for short period hot-Jupiter type planets. Here we present the latest results and updates from the most recent engineering and observing runs with the multi- object Keck ET. P23 Notes: New Results from Observations of Massive Star Formation in the Mid-Infrared with Large Aper- ture Telescopes James De Buizer Gemini Observatory Recent observations in the mid-infrared (5-25 um) of massive young stellar sources have yielded a surprising result: many show evidence of mid-infrared emission from outflows and jets. 39 P25 Notes: High Contrast Imaging with the Hale 200” Tele- scope at Palomar Justin Crepp; Joseph Carson; Gene Serabyn; Jian Ge; Ivan Kravchenko University of Florida We present recent work on a high-contrast imaging effort that is designed to image sub-stellar companions orbiting nearby stars. Our technique is to generate Strehl ratios that exceed 90% at near-infrared wavelengths (1.90-2.30 micron) by effectively turning the Hale 200” (5.093 m) telescope into a smaller (1.5 m diameter) off-axis imager. To eliminate unwanted diffraction, P27 the subsequent circular subaperture conveniently avoids the High resolution spectroscopy of planet bearing telescope central obstruction and spiders, and is then magnified stars and reimaged via relay optics onto the AO system deformable mirror. The starlight then passes through a Lyot coronagraph M.C. Galvez; J. Ge that is equipped with the same technology that currently repre- University of Florida sents the baseline design for the Terrestrial Planet Finder-Coro- We present here the first steps of an extended spectroscopic sur- nagraph, namely a notch-filter image mask, which is manufac- vey in order to characterize stellar hosts of extra-solar planets. tured with nanoscale precision using electron-beam lithography. We have selected several known stars with planets and using This combination of off-axis design, high-order AO, and state-of- high resolution spectroscopy, we have studied their properties. the-art coronagraphy, can, in principle, generate contrast levels on the order of 10-5 (i.e. ~12.5 magnitudes) at sub-arcsecond Notes: separations. Notes:

P28 P26 High-resolution Mid-IR Imaging of Herbig Ae/Be stars: Morphology of the Circumstellar Dust Cataclysmic vs. continuous collisions in debris disks: a study of the resolved disk of Zeta Lep N. Mariñas; C. M. Telesco; R. S. Fisher; C. Packham University of Florida Moerchen, M. M.; Telesco, C. M.; Packham, C. C.; R. S. Fisher University of Florida We have imaged the circumstellar environments of 22 nearby Herbig Ae/Be stars (pre-main sequence stars of intermediate mass) Debris disks surrounding main-sequence stars emit excess infra- in the mid-IR using the Gemini North and South telescopes. All red flux due to scattered light from dust in the near-infrared and sources included in this sample are optically visible Herbig stars, thermal re-radiation from dust in the mid-infrared. The debris that have been sub-classified as either group I sources, which disk of Zeta Lep, an A-type main-sequence star 21.5 pc from the have almost flat spectral energy distribution in the mid-infrared, Sun, was discovered by IRAS in 1991 to have a strong infrared or group II sources, which exhibit a decline towards the far-in- excess, which has been confirmed recently with Spitzer photom- frared. Since mid-IR emission traces the dust hotter than 100 K, etry and is unusually bright for a disk of its estimated age (~300 our survey sensitivity and spatial resolution allow us to directly Myr). It is well known that, for dust to be present in quantities explore the morphology of the circumstellar emission in these capable of producing such excess emission, it must be supplied systems within a couple hundreds of AU from the central star and continuously through collisional cascades and related process- discriminate between flaring disk geometries, which have been es. Using high-resolution (~0.5”) mid-infrared imaging at Gem- linked to group I sources, and self-shadowed disks thought to be ini, we are exploring these ongoing physical processes within a group II sources. We spatially resolve 9 of the 11 group I sources, sample of known debris disks including Zeta Lep, which is the while all the group II sources show compact unresolved mid-IR first disk in our sample that we have clearly resolved. Quadratic emission. In the case of the two unresolved group I sources, the subtraction of the PSF star from the source indicates a scale size distance to one of the sources has been recently corrected from for the disk of ~3 AU from the central star. I will describe the 164 pc to over 400 pc, placing this source beyond our spatial grain properties that can be inferred from our mid-IR observa- resolution limit. We believe the other unresolved group I source tions along with a comparison of two scenarios for the produc- has been misclassified using the IRAS fluxes; our mid-IR fluxes for tion of the observed emitting dust. The comparable size of this this source are almost a factor of 100 lower at 12 microns, and disk to that of our asteroid belt presents evidence for a new disk the source is not detected at 18 microns. We have found a strong archetype -- in contrast to more greatly extended Kuiper Belt correlation between the two groups classification and intrinsic analogs such as Beta Pic -- which may explain some debris disks spatial differences in the distribution of the circumstellar dust. that high resolution imaging observations cannot yet resolve.

40 Notes: Notes:

P29 P31 FLAMINGOS Spectroscopy of Low Mass Stars and Stochastic Collisional Events in Debris Disks: Brown Dwarfs in Orion What can be Learned from the Zodiacal Cloud? Rashkind, N.; Levine; J. L., Steinhauer; A.; Lada, E. A. Thomas J. J. Kehoe; Stanley F. Dermott; Charles M. Telesco University of Florida University of Florida In this poster we present results from a near-infrared spectro- Debris disks are composed of dust particles that are not pri- scopic survey of young embedded clusters in the Orion molec- mordial but are continually replenished by the erosion of their ular cloud complex. These data were obtained as part of the planetesimal populations, either as a result of collisional destruc- FLAMINGOS/NOAO survey of the star forming content of the tion or cometary activity. These debris disks therefore provide a five nearest giant molecular clouds. All data were obtained using natural laboratory for studying the physical processes that occur FLAMINGOS the KPNO 2.1m and 4m telescopes. We use spec- during the birth and evolution of planetary systems. The solar tra to determine effective temperatures for a magnitude-limit- system’s debris disk, better known as the zodiacal cloud, is just ed sample of cluster sources. These data were then combined an example of a debris disk that is much older than those that are with FLAMINGOS J, H, and K-band photometry to determine typically observed around stars other than the Sun. The results bolometric luminosities and then place all objects on the H-R of ongoing collisional activity within planetesimal populations in diagram. The data are then compared to current pre-main se- the solar system can be seen today in the form of asteroid families quence evolutionary models and we estimate masses and ages and the solar system dust bands discovered by the IRAS. These for all objects. Finally, we examine the star forming history of objects are composed of material from opposite ends of the size the region and investigate the significance of the brown dwarf spectrum of collisional debris released as a result of the disrup- population. tion of an asteroidal parent body. In fact, several very young asteroid clusters, less than 10 million years old, have recently Notes: been discovered and some of these have now been identified as sources of the IRAS dust bands. The orbits of the particles com- prising the dust bands decay as a result of Poynting-Robertson drag and solar-wind drag, causing the dust particles to spiral in towards the Sun on timescales than can be much shorter than this. This implies that we currently observe only the tail-end of an initially much larger flux of particles. Earth accretes some of these particles as they evolve inward and so evidence of the in- tense dust showers resulting from past catastrophic collisional events in the asteroid belt is likely preserved in the geologic record. As in the young solar system, planetesimal populations P30 around other stars probably undergo an intense period of vio- Differential Imaging Adaptive Optics observations lent collisional evolution during the planet formation epoch that of the protostar Elias 2-29 results in the bright debris disks that can be observed at mid-IR N. Huelamo; W. Brandner; S. Wolf wavelengths. Moreover, recent observational evidence supports Observatorio de Lisboa the hypothesis that even mature systems that still contain belts of planetesimals could occasionally and unexpectedly flare into We present dual imaging Adaptive Optics (AO) observations of infrared visibility due to the stochastic catastrophic disruption Elias 2-29, a protostar in the Rho Ophiuchi star forming region. of those planetesimals, in events similar to those that generated The target is surrounded by a disk (and possibly by an envelope) the solar system dust bands. The existence of a comprehensive but it has not been spatially resolved so far. We have obtained dataset of observations of the zodiacal cloud enables us to tightly dual imaging polarimetric observations with a Wollaston prism constrain our models and better understand the origin, struc- using NAOS-CONICA, the AO facility and infrared camera at ture, and evolution of mature debris disks. the VLT. This technique provides high contrast images given that the contribution of the speckle noise is significantly reduced. Notes: Our H and K-band observations show the presence of a highly inclined circumstellar disk, which is spatially resolved in polar- ized light. The physical properties of the circumstellar disk will be derived by comparison with theoretical models.

41 P32 lar component of the Groth field, explaining the calibration and TRACING TIDAL STREAMS WITH GTC: TESTING THE HIER- selection of point sources methods used. Also, we compare with ARCHICAL FORMATION OF THE MILKY WAY models of stellar population synthesis of the Galaxy. David Martinez-Delgado Notes: Instituto Astrofísica Canarias Within the hierarchical framework for galaxy formation, galax- ies are expected to form and evolve through mass infall and through the successive coalescence of smaller, distinct building blocks, such as satellite galaxies merging with their parent gal- axy. This framework predicts distinct tidal stellar streams in and around large galaxies and at r>10 kpc such streams should re- main detectable as coherent stellar over-densities for billions of years. In the last years, different large scale CCD surveys (Sloan Digital Sky Survey, 2MASS, QUEST) have probed for the first time the presence of a significant amount of these substructures in the halo of the Milky Way (MW) in form of long tidal streams P34 or stellar clumps which have been interpreted as the fossil re- VLT Spectroscopy of Massive Stars in NGC55 cords of the hierarchical Galaxy formation. On the other hand, Norberto Castro Rodriguez; Artemio Herrero Davo; Carrie Trun- N-body simulations of these merger events have also been ex- dle: Fabio Bressolin: Miriam Garcia tensively used to associate detected tidal debris with their dwarf Instituto de Astrofisica de Canarias progenitor galaxies with the aim of constraining the dynami- cal history of the progenitor satellites and the properties of the We present optical VLT spectroscopy of massive stars in NGC55, MW’s dark matter halo. a nearby spiral galaxy located at about 2 Mpc. The data, taken with FORS2 (3300-6210Å, l /Dl =780) in MXU mode, allow This observational and theoretical effort has led to an compre- us to provide spectral classification for approximately 200 ob- hensive understanding of the two largest tidal streams discov- jects located throughout the galaxy. From this sample, suitable ered so far in our Galaxy: the tidal stream of the Sagittarius dwarf B-type supergiants are chosen for subsequent higher resolution galaxy, which wraps the MW in an almost polar orbit ( Martínez- spectroscopic observations that will enable the determination Delgado et al. 2001; Majewski et al. 2003) and the Monoceros of their chemical composition. The stellar abundances derived tidal stream (Yanny et al. 2002; Ibata et al. 2003), a low-latitude for objects located across the galaxy provide information of the tidal stream whose progenitor moves on a prograde, nearly cir- metallicity gradient of NGC55, a key point in the study of the cular orbit (Peñarrubia, Martínez-Delgado et al. 2005). galactic evolution. We also discuss how the enhanced sensitivity In this talk, I present a long term project that exploits the exqui- and spectral resolution of GTC-OSIRIS can be a valuable tool for site image quality of the Gran Telescopio de Canarias to confirm similar studies in galaxies, both in the Local Group and beyond. the presence and origin of numerous stellar over-densities de- Notes: tected in the Galactic halo, that could be related with the fos- sil records of the hierarchical formation of the Milky Way. The ultimate objective of this project is to complete the census of merger events in our Galaxy, which can be directly compared with the predictions of the Cold Dark Matter cosmological mod- els (Bullock et al. 2004). Notes:

P35 VLT Spectroscopy of Massive Stars in NGC55 Norberto Castro Rodriguez; Artemio Herrero Davo; Carrie Trundle; Fabio Bressolin; Miriam Garcia Instituto de Astrofisica de Canarias We present optical VLT spectroscopy of massive stars in NGC55, a nearby spiral galaxy located at about 2 Mpc. The data, taken P33 with FORS2 (3300-6210Å, l /Dl =780) in MXU mode, allow us to provide spectral classification for approximately 200 objects The OTELO project: Stellar component in the located throughout the galaxy. From this sample, suitable B- Groth field type supergiants are chosen for subsequent higher resolution 1 Ana M. Pérez-García; Emilio Alfaro; Jordi Cepa ; Ángel Bon- spectroscopic observations that will enable the determination giovanni; Héctor Castañeda; Jesús Gallego; Ignacio González- of their chemical composition. The stellar abundances derived Serrano; J. Jesús González-González; Miguel Sánchez-Portal for objects located across the galaxy provide information of the 1 Instituto Astrofísica Canarias metallicity gradient of NGC55, a key point in the study of the We present the results of the analysis of the broad band images galactic evolution. We also discuss how the enhanced sensitivity of the Groth field. This broad band survey was carried out with and spectral resolution of GTC-OSIRIS can be a valuable tool for the 4.2m WHT at La Palma. In particular, we analyze the stel- similar studies in galaxies, both in the Local Group and beyond. 42 Notes: P37 Searching with GTC for the carrier of the Anoma- lous Microwave Emission Susana Iglesias-Groth Instituto Astrofísica Canarias Several recent experiments have shown evidence for the exis- tence of a new microwave emission process in our Galaxy (in the range 10-60 GHz) that may affect the ability to infer cosmologi- cal parameters from the Cosmic Microwave Background with the aimed precision of 1%. This emission process has been iden- P36 tified in the Perseus Molecular Complex in dark clouds (like LDN Studying the Wake of the Galactic Center Source 1622) and as a diffuse component at high Galactic latitudes (Fer- IRS8 nandez-Cerezo et al. 2006). The carrier of this emission process R. Scott Fisher; Tom Geballe; Jean-Rene Roy is not identified yet. It could possibly be related to hydrogenated Gemini Observatory carbon molecules (PAHs and/or fullerenes) fast rotating in those environments and emitting electric dipole radiation. These mol- In the mid-IR the signature of the dust in the Galactic Center ecules could also be characterized by optical and infrared transi- (GC) is unmistakable. Along with a region of complex extend- tions. We plan to observe with GTC (OSIRIS) selected hot stars ed emission there are at least 15 very bright point-like mid-IR located behind regions where clear anomalous emission have sources within a radius of ~3 pc from the central 2x106 solar been detected in order to detect optical transitions associated to mass black hole (named Sgr A*). One of the most unusual of the carriers of this emission. In addition, with CANARICAM we these bright mid-IR sources is IRS8 which is located 30” north aim to characterize the possible thermal infrared emission lines of Sgr A* in the ‘suburbs’ of the GC. Because of its relatively of the carrier in several dark clouds. The detection of diffuse remote location with respect to the other GC sources, IRS8 has interstellar bands and thermal infrared lines in regions where not been studied extensively. Indeed, it was a somewhat seren- anomalous microwave emission is dominant will possibly be key dipitous discovery when Geballe et al. (2004) first saw a detailed to establish the nature of the responsible particles. bow shock of emission associated with the source during SV ob- servations with the near-IR adaptive optics system Hokupa’a on Notes: Gemini North. Here we present preliminary results from our study of this source in the mid-IR with the Gemini instruments T-ReCS and MICHELLE. Our imaging with T-ReCS complements the near- IR data of the discovery paper as it conclusively shows that the bow shock and photosphere of IRS8 are heating the nearby dust to temperatures of several hundred Kelvin. We will also present low and high resolution spectroscopy from MICHELLE. Our low resolution spectra (R~150) show that there is little crystalline P38 silicate dust near IRS8, implying that the hard radiation field of First Infrared Spectroscopic Identification of a the star is not actively processing any of the ambient ISM dust Chandra Low-Luminosity X-ray Source in the Ga- into crystalline grains. Our high resolution spectra (R ~30000), lactic Center centered on the Ne[II] line at 12.8 um, allow us to study the de- Valerie J. Mikles; Stephen S. Eikenberry; Michael P. Muno; tailed kinematics of the source by revealing the complex velocity Reba M. Bandyopadhyay; Shannon Patel structure of the gas within and near the IRS8 bow shock. University of Florida This research is presented to highlight the capabilities of mod- We present the first results of a campaign to find and identify ern facility-class instruments on a 8-10m class telescope. Given new compact objects in the Galactic Center. Selecting candi- that CANARICAM has similar capabilities to both T-ReCS and dates from a combination of Chandra and 2MASS survey data, MICHELLE (including imaging and spectro-polarimetry) the GC we search for accretion disk signatures via infrared spectroscopy. region and IRS8 itself will be obvious targets for more in depth We have found the infrared counterpart to the Chandra source studies with the GTC. CXO J174536.1-285638, the spectrum of which has strong Notes: Brackett series and HeI emission. The presence of CIII, NIII, and HeII indicate a binary system. We suggest that the system is some form of high-mass binary system, either a high-mass X-ray binary or a colliding wind binary similar to Eta Carinae. This is the first spectroscopically confirmed counterpart to a Chandra low-lumi- nosity X-ray source. Notes:

43 P39 Notes: Calcium II Triplet Abundances for a Sample of LMC Clusters Aaron J. Grocholski; Andrew A. Cole; Ata Sarajedini; Doug Geisler; Verne V. Smith University of Florida Results from our spectroscopic survey of populous clusters in the LMC are presented. In an effort to update previous metal- licity determinations, we have utilized FORS2 (in MXU mode) on the Very Large Telescope to obtain near infrared spectra for more than 200 stars in 28 populous LMC clusters. This cluster P41 sample spans a large range of ages (~1-13 Gyr) and metallicities The stellar structures around disk galaxies (-0.3 > [Fe/H] > -2.0) and has good areal coverage of the LMC disk. The broad absorption lines of the Calcium II triplet (CaT) Igor Drozdovsky; Antonio Aparicio; Carme Gallart; Sebastian are used to derive cluster radial velocities and abundances; for Hidalgo; Matteo Monelli; Eduard Bernard; Nikolay Tikhonov; eight of these clusters, we report the first spectroscopically de- Olga Galazutdinova termined metallicities based on individual cluster stars, and six Instituto de Astrofisica de Canarias of these eight have no published radial velocity measurements. I’ll present a summary of our systematic and homogeneous This work is supported by NSF CAREER grant AST-0094048 to analysis of the surface number counts and population gradients Ata Sarajedini. of the resolved stars in surroundings of the nearby disk galax- ies, observed with space- (Hubble & Spitzer) and ground-based Notes: telescopes. We examine the radial (in-plane) and vertical (ex- traplanar) distributions as a function of stellar age by tracking changes in the color-magnitude diagram of face-on and edge-on galaxies. Our data show that the scale length and height of a stel- lar population increases with age, with oldest of the detected red giant branch population (RGB) identified at large galactocentric radii or extraplanar height, out to typically a few kpc. In the most massive of the studied galaxies there is evidence for a break in number density and color gradients of evolved RGB stars, which plausibly correspond to the thick disk and halo components of the galaxies. The results may imply that all massive spiral galaxies not only have a thick disk but also poses an extended halo, while P40 dwarf disk galaxies have solely a thin/thick disk component. However, our photometric data need to be complement with The Mid-Infrared Emission of M87 kinematic information of these stars that can be provided my E. Perlman1; R. Mason2; C. Packham3; J. Schaefer3; J. Radom- multi-object spectrographs on 10-m class telescopes. The fea- ski4; M. Imanishi5; N. A. Levenson6; M. Elitzur6; W. Sparks7 sibility of the radial velocity observations based on the strength 1University of Maryland, Baltimore County; 2NOAO Gemini Sci- of the near-infrared calcium triplet will be discussed. This type ence Center; 3University of Florida; 4Gemini; 5NAOJ; 6University of of analysis will allow us to shed light on fundamental questions Kentucky; 7STScI about the evolution of disk galaxies, such as disk heating versus We discuss imaging and spectroscopy of M87 in the mid-infra- merger scenarios and a role of these mechanisms in forming the red, using observations with Subaru and the Spitzer Space Tele- stellar disks and halo. scope. Our previous work showed that at N band the nucleus of Notes: M87 is dominated by the AGN point-source, but was marginally resolved. The Spitzer data include high signal-to-noise spectra of both the nucleus between 5-35 microns, and of the knot A/B complex between 15-35 microns, while the Subaru data contain imaging, plus spectroscopy of the nucleus only between 8-13 microns. As expected, the spectrum of the knot A/B complex is consistent with synchrotron emission from components in the jet. However, a single-component synchrotron model cannot account for the IR continuum from the nucleus, even when contributions to the spectra from components in the jet (due to the degrading of resolution with wavelength) are included. We P42 model the extra long-wavelength flux as thermal emission from cool dust at a temperature of about 60 K, with an IR luminos- Studying Galaxy Formation and Evolution from ity of 4 x 1038 erg s-1. We also find several emission lines from the Local Group galaxies low-ionization species in the nuclear spectrum. We discuss the C. Gallart; A. Aparicio; E. Bernard; R. Carrera; I. Drozdovsky; implications of these findings for our understanding of M87 and S. Hidalgo; A. Mar’in-Franch; I. Meschin; M. Monelli; N. Noel; also for unified AGN models. A. Rosenberg Instituto de Astrofisica de Canarias The Local Group galaxies can be studied in great detail from their resolved stars, and thanks to the current superb observing 44 facilities, and theoretical modeling. We plan to study the gal- P44 axy formation and evolution process through a comprehensive Results of high-spatial resolution mid-IR imaging study of Local Group galaxies. To accomplish this goal, we plan of NGC7172: and the Discussion and Applicication to use a number of complementary tools which will allow us to of Results From the Development of mid-IR Data study the two main mechanisms that determine galaxy forma- Refinement Techniques tion and evolution, namely: 1. The star formation history, and Justin J. Schaefer; Chris. P. Packham; Charles M. Telesco; James its influence on galaxy evolution, through: - The study of deep T. Radomski color-magnitude diagrams of each galaxy; - The spectroscopic University of Florida abundances of resolved stars; -The analysis of the properties of their variable stars; -The study of the Milky Way Cluster system. We present results from an analysis of high-spatial resolution im- 2. The mass assembly and the dynamical evolution of each sys- ages of the Seyfert 2 galaxy NGC7172 (0.09”/pixel), as observed tem, through: -The stellar population gradients and kinematics by T-ReCS on Gemini South at 10 microns. We discuss emission of stars of different ages; -The dynamics of the Local Group and contributions of the galaxy and the nucleus to the mid-IR image, the influence of interactions on galaxy evolution. and use archival data to examine the spectral energy distribution of this galaxy. In particular, we discuss the contributions of the This project is designed in order to make an excellent use of GTC unresolved nuclear bulge and ionization cones to the observed and its first light instruments, in special OSIRIS. In this Poster, 10 micron flux. We then present the results of a mid-IR noise we present examples of ongoing research on the sub-projects reduction technique, and demonstrate its application to images above. which have chop/nod subtracted residual noise. Notes: Notes:

P43 P45 High Resolution Mid-Infrared Imaging of Seyfert Galaxy Cluster Assembly at z ~ 0.37 Nuclei: Current Results and the Future with Ca- nariCam on the GTC Lauren Davis; Anthony Gonzalez University of Florida James Radomski; Chris Packham; Charles M. Telesco Gemini Observatory We present new results from a multiwavelength study of the su- pergroup SG1120-1202. Consisting of at least four gravitation- The study of Active Galactic Nuclei (AGN) represents a signifi- ally bound galaxy groups at z = 0.371, the supergroup will merge cant area of research in astrophysics. Thought to be primarily to form a cluster with a mass of approximately that of the Coma powered by a supermassive black hole these objects can pro- cluster by z ~ 0. This system presents a unique opportunity to duce thousands of times more energy than the entire Milky Way study the impact of cluster assembly on the morphologies and galaxy on scales smaller than our solar system. A subset of these star formation rates of group galaxies. Data are avalable from galaxies, Seyferts, represents the closest species and thus pro- the HST, Chandra, Spitzer, and ground based optical and infra- vides an ideal laboratory to study not only this subclass of AGN red; we determined group membership using optical spectros- but also the phenomena as a whole. Buried deep in the centers copy from Magellan and VIMOS on the VLT. We are now initiat- of galaxies, mid-infrared imaging provides and ideal approach ing work to explore the correspondence between star formation to studying Seyfert nuclei which may be completely obscured at rates derived from optical spectroscopy and MIPS observations optical wavelengths. The mid-IR traces multiple emission mech- to determine the total star formation rate in this system. Finally, anisms associated with AGN including emission from a dusty we note that OSIRIS and EMIR on the GTC will provide a valu- torus surrounding the central black hole and circumnuclear able means of expanding upon our current program by supply- starburst activity. In this talk I will highlight the results of an on- ing the imaging and multi-object spectroscopy necessary for an going high spatial resolution mid-IR imaging survey of Seyferts extension of the program to the surrounding environment. and discuss the future of such research with CanariCam on the GTC. Notes: Notes:

45 P46 ling individual AGN, including the optical depth per cloud, the The Stellar Populations of M33’s Outer Regions number of clouds along the line of sight, the radial variation and height of the distribution, and the viewing angle. We can also re- Michael Barker; Ata Sarajedini; Doug Geisler; Paul Harding; cover the intrinsic AGN luminosity in the type 2 sources, where Robert Schommer it cannot be measured directly. We apply these diagnostics to University of Florida observations of NGC 1068. Studying the stellar populations in the outskirts of spiral galaxies We demonstrate that in general the mid-IR emission is anisotro- can provide important constraints on their structure, formation, pic on small scales, which may be discerned in nearby, luminous and evolution. To that end, we present deep HST/ACS photom- examples. In all cases, however, the dominant emission is con- etry of three fields located at deprojected radii of ~6 - 9 K-band fined to very small physical scales, even though the total extent scale-lengths southeast of M33’s nucleus. The radial distribution of the cloud distribution may be large. of stellar surface density declines exponentially High spatial resolution is essential to isolate the immediate cir- with increasing galactocentric distance which is indicative of a cumnuclear region from larger-scale emission. The Gran Tele- disk population. The color-magnitude diagrams (CMDs) reveal scopio CANARIAS with CanariCam will be ideally suited to a population with a mix of ages from ~100 Myr to ~10 Gyr. The obtain these sensitive data. In the future, we will measure true red giant branch metallicity decreases from -1.1 to -1.3 across all samples of many galaxies to understand the obscuration of AGN three fields, a gradient consistent with that of M33’s inner disk. more generally, rather than rely on isolated examples of excep- We also present preliminary results on the star formation history tional sources. of these fields using the technique of synthetic CMD fitting. Notes: Support for this work (proposal number GO-9479) was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. Notes:

P48 Mid-IR studies of nearby AGN at high spatial reso- lution R. Mason; C. Packham; N. Levenson; T. Geballe; M. Elitzur; J. Radomski; S. Fisher; E. Perlman; A. Petric; G. Wright P47 Gemini Observatory Measuring the Inhomogeneous Obscuration of The unified model of active galactic nuclei (AGN), which ex- AGN with Mid-Infrared Observations plains the differences between types 1 and 2 AGN with a to- N. A. Levenson; M. Elitzur; T. R. Geballe; R. E. Mason; M. Nen- roidal cloud of dust and gas that obscures the broad line gas kova; M. M. Sirocky from some viewing angles while leaving it exposed from oth- University of Kentucky ers, brought some much-needed order to the active galaxy zoo. The detection of broad emission lines in polarised light in many Accretion onto supermassive black holes is the energy source of Seyfert 2 galaxies demonstrates the basic validity of the model, active galactic nuclei (AGN), and many of the diverse observed but many questions remain as to the precise nature (extent, ge- characteristics of AGN can be accounted for in terms of varia- ometry, dust properties...) of the obscuration and the extent to tions in viewing geometry toward this common central engine. which this simple model can really account for the differences The intrinsic hard emission must be blocked from some lines between the AGN types. of sight, and it is reprocessed to emerge at infrared (IR) wave- lengths. IR observations therefore provide the best probes of the The dusty “torus” will strongly absorb UV/visible radiation from obscuring region itself. the nucleus and re-emit it in the mid-IR, so observations at these wavelengths, and in particular of the strong Si-O bond stretch Despite the successes of existing ``unified AGN models,’’ cur- around 10 microns, can provide strong constraints on models rent data reveal several problems with descriptions that include aiming to explain and predict the emission from AGN. Further- a homogeneous obscuring torus. First, X-ray data indicate a more, observations from the largest ground-based telescopes are wide range of column densities along the line of sight, while starting show that the MIR-emitting regions of these objects can the IR spectral energy distributions show little variation. Second, be highly complex – the spatial resolution currently obtainable uniform models predict silicate emission around 10um in all di- only from the ground is a crucial complement to sensitive Spitzer rectly-viewed (type 1) sources, and absorption in all obscured observations of active galaxies. Here we present high-resolution (type 2) sources. The emission is in fact detected from only a MIR observations of two nearby galaxies that tackle issues as di- small number of type 1 sources, and the depth of the feature verse as the contribution of the torus to the small-aperture MIR is not strongly correlated with the total obscuration of type 2 emission, the AGN-starburst connection, and the application of sources. the unified model to very low-luminosity AGN. The combination Recent models of inhomogeneous obscuration by large optical of resolution and sensitivity expected from CanariCam on the depth clouds solve these problems. Mid-IR spectroscopy and GTC will provide a valuable opportunity to further explore the imaging may then constrain the physical parameters in model- avenues opened up by this early research. 46 Notes: P50 Optical Variability of Infrared Power Law-Select- ed Galaxies & X-ray Sources in the GOODS South Field Alison Klesman; Vicki Sarajedini University of Florida This study investigates the use of optical variability to identify AGN in the GOODS South field. Photometry was performed on a sample of 23 infrared power law-selected AGN candidates and 83 X-ray sources with optical counterparts. Each object is classi- fied with a variability significance value, which is related to the P49 standard deviation of its magnitude in five epochs separated by 45-day intervals. The variability significance is compared to IR Spatially-resolved mid-infrared spectroscopy of and X-ray properties of the sources. We find that the majority IC 5063 of high-significance variables are consistent with IR spectral en- Stuart Young; Christopher Packham; James T. Radomski; ergy distributions typical of BLAGNs and are usually softer X-ray Charles M. Telesco sources. Nonetheless, 30% of the IR-selected AGN candidates University of Hertfordshire without X-ray emission, generally thought to be highly obscured IC 5063 (PKS 2048-572) is a nearby (z=0.011) narrow-line radio sources, are significantly to marginally variable in the optical, galaxy resident in what is usually classified as an S0-type gal- confirming their AGN nature. axy. A prominent dust lane is observed partially covering the Notes: eastern half of the host galaxy. With a radio power that is about two orders of magnitude greater than nearby Seyfert galaxies, IC 5063 is in the range of low-luminosity radio elliptical galaxies. The optical spectrum is dominated by relatively narrow emis- sion lines and narrow band imaging reveals an extended nar- row line region aligned with the extended radio emission at a position angle of approximately 303 degrees (Colina et al. 1991). The discovery of scattered broad lines observed in polarized flux (Inglis et al. 1993) revealed the presence of an obscured type-1 nucleus, the first observation of this phenomenon in an interme- diate power radio galaxy. P51 Here we present spatially-resolved, near-diffraction-limited 10 Stellar Populations in Luminous Compact Blue micron spectra of the nucleus of IC 5063, obtained with Ther- Galaxies mal-Region Camera Spectrograph (T-ReCS), the mid-IR imager and spectrometer on the 8.1 m Gemini South telescope. The Carlos Hoyos; Ángeles I. Díaz; Rafael Guzmán; David C. Koo; slit was aligned along the direction of the cone of narrow-line Matthew B. Bershady emission. The spectra cover the nucleus and the inner reaches Universidad Autónoma de Madrid of the ionization cones at a spatial resolution of approximately We investigate the star formation history and stellar populations 0.4 arcsecs (90 parsecs). Spectra extracted in steps along the slit of four Luminous Compact Blue Galaxies (LCBGs) at intermedi- reveal variations in continuum slope and silicate feature profile ate redshift using evolutionary population synthesis techniques. and depth on subarcsecond scales, illustrating in unprecedented The derived stellar generations and star formation histories are detail the complexity of the circumnuclear regions of this galaxy compared to those of other local systems, including H-II galax- at mid-IR wavelengths. The dust population in the region of the ies and Blue Compact Dwarves. We find that the first episodes narrow-line region is significantly warmer than that to the SE of of star formation these systems underwent happened at z=0.7. the nucleus. This is consistent with an observation of the cooler The stellar populations found are similar to the ones found in HII dust present in the outer reaches of the postulated torus that galaxies but not to BCDGs. The HI and dark matter content are obscures the type-1 nucleus in this object. thought to be small. This particular sample of LCBGs can evolve Notes: to a dE or Sph stage, provided that there are no further star forming episodes. The data on the LCBG sample were obtained with the WFPC2 and STIS instruments on board the Hubble Space Telescope (HST). Notes:

47 P52 P54 Merger fraction in Groth strip SMBH-Host Galaxy Evolution at High Redshifts Lopez, Carlos; Balcells, Marc; Prieto, Mercedes Fred Hamann; Craig Warner; Matthias Dietrich; Linda Watson Instituto Astrofísica Canarias University of Florida At the moment exist two principal theories to explain the for- Super-Massive Black Holes (SMBHs) are common and prob- mation of local structures and galaxies: the hierarchical model, ably inevitable byproducts of galaxy formation. Recent studies which supposes a low-z formation of the most massive galaxies indicate that every massive galaxy has an SMBH in its core and, by mergers and the monolithic model, which supposes a high-z moreover, that the mass of the SMBH scales directly with the formation of those galaxies and the subsequent passive evolu- mass of the host galactic spheroid. There is, in addition, a well- tion. established positive correlation between galaxy mass and galaxy metallicity. However, both of these relationships to galaxy mass One of the parameters that can inform us about which model have been studied so far only at ~zero redshift (i.e., in present- is the most important in the galaxy formation is the merger frac- day galaxies). To examine these relationships at high redshifts tion (fmg) and his change with the redshift. Fmg is defined as and study their evolution across cosmic time, we have begun a the ratio number of merger galaxies/total number of galaxies. program of spectroscopic emission-line observations of AGNs at In this poster we present the first results in the determination both “low” (z < 0.5) and high (z > 1.8) redshifts that have pub- of fmg evolution from the GOYA Survey, in the Groth strip. We lished imaging data of their host galaxies (e.g., with the Hubble obtain the fmg in two ways: 1) Study of merger galaxies with the Space Telescope). The combined dataset will test the hypothesis automatic morphological CAS system; 2) Study of pair galaxy that the gas-phase metallicities near AGNs also scale with host counts. galaxy mass by making the first direct comparison between these two quantities. We will also examine the M_BH versus M_bulge In this study we use a Ks-band selected catalog, because we relationship, and compare critical AGN properties (such as want to calibrate the fmg with the mass of the galaxies, which is SMBH mass, metallicity, and the accretion diagnostic L/L_edd) better reproduced by this band. to host luminosity/mass, over ~7 Gyr of cosmic time - thus pro- Notes: viding key constraints on coupled AGN-SMBH-galaxy evolution. Finally, we will compare the SMBH masses derived from the H- beta and CIV 1549A emission lines, and compare both to the host galaxy luminosities, to calibrate the use of CIV as a mass diagnostic at high redshifts. This work lays the groundwork for future large AGN/galaxy surveys, such as GOYA with the GTC. Notes:

P53 Ks band-selected galaxy catalog 0 < z < 5 David Abreu; Marc Balcells; Cesar E. García; Mercedes Prieto; Carmen Eliche Instituto Astrofísica Canarias The redshift-evolution of the K-band luminosity function (LF) of galaxies provides important empirical information on the rate P55 of mass assembly of galaxies. Using the GOYA Survey UBVIJK The object selection for the GOYA survey imaging of the Groth strip, we have defined a catalog of distant galaxies limited by K-band flux. 2400 galaxies were detected in Guillermo Barro Calvo; Jesus Gallego; Jaime Zamorano; Vic- K over the 133 sq. arcmin of the HST/WFPC2 mapping of the tor Villar Groth strip, and aperture photometry is available for the remain- Universidad Complutense de Madrid ing bands. Photometric redshifts (HyperZ) could be derived for I will present my current thesis work about the preliminar stud- ~2000 sources in the range 0 = The Goya survey, is one of the GTC scientific projects, which 0.07. Such catalog will provide a robust determination of the aims to study the properties of galaxies at high redshift using the evolution of the K-LF, as well as the galaxy mass function, to NIR multi-slit spectrograph which is being constructed for GTC z~1.5. (EMIR). Notes: In particular, to study the galactic evolution, GOYA will carry out an spectroscopic study of the emission-line galaxy population at the 1.4-2.8 redshift range, and given that EMIR will provide NIR spectroscopy for up to 50 targets, to obtain a wide sample of se- lected galaxies will be a key part of the project, which has to be performed before the first light of the instrument. Our work on the target selection follows two different approach- es: (1) Reducing and extracting catalogs from deep K-band in- frared images on the Groth strip, to provide nIR data for photo- 48 redshift calculations, and (2) designing and interactive database at different redshifts, and about 0.5% galactic emission stars. The for the GOODS fields (HDF-N and CDFS), based on public multi spectra extracted from the data cubes will allow deblending the wave length information, which will provides us with a fast in- Ha from the [NII]658.3,654.8 nm lines, thus allowing an estima- terface to obtain samples of galaxies that fulfill the requirements tion of the metal contents of the targets and the possibility to of the GOYA survey. discriminate between the various AGN types. An auxiliary UB- VRIJK broadband survey of the OTELO fields, currently under Notes: way, will allow, through photometric redshifts, the identification of the emission lines detected, as well as a morphological clas- sification of the emitting sources. Notes:

P56 GTC follow-up of AzTEC sources: probing high-z dusty starbursts P58 Itziar Aretxaga; AzTEC team The OTELO project: deep X-ray and optical observa- INAOE tions of the Groth strip AzTEC is the 144 pixel 1.1/2.1mm bolometer camera of the 50- Miguel Sánchez-Portal; Ana M. Pérez-García; Mirjana Povic; Jor- m Large Millimeter Telescope that, previous to installation in its di Cepa; Emilio Alfaro; Ángel Bongiovanni; Héctor Castañeda; final home, has now completed its first scientific run on the 15m Jesús Gallego; Ignacio González-Serrano; J. Jesús González- JCMT. We describe the instrument, its first scientific run that car- González ried out both galactic and extragalactic projects, and focus on Instituto Astrofísica Canarias the follow up of the AzTEC high-z galaxies that the GTC will be We present a preliminary analysis of public, deep (200 ksec) able to accomplish. Chandra/ACIS observations of three fields comprising the origi- Notes: nal Groth-Westphal strip, gathered from the Chandra Data Ar- chive, combined with optical VRI data from our broadband survey carried out with the 4.2m WHT at La Palma. Several distance-independent diagnostic tools are applied, including the X-ray to optical flux ratio (X/O) and hardness ratios (HR). The optical properties (B/T ratio, colours) of the X-ray emitters are reviewed. Notes:

P57 The OTELO project Jordi Cepa; Emilio Alfaro; Angel Bongiovanni; Héctor Casta- ñeda; Jesús Gallego; J.I. González-Serrano; J.J. González; D. Heath Jones; A.M. Pérez-García; Miguel Sánchez-Portal Instituto Astrofísica Canarias OTELO, the key OSIRIS science project, is a deep emission line object survey to be performed with the OSIRIS Tunable Filters, P59 in selected atmospheric windows relatively free of sky emission A Survey of Quasars and their Host Galaxies at lines. The observing strategy will allow studying a clearly defined High Redshift volume of the Universe at a known flux limit. The total survey Leah Simon; Fred Hamann sky area is about 1 square degree, distributed in different high University of Florida latitude and low extinction fields with adequate angular separa- tions. The survey will result in 3D data cubes covering 150+180 Quasars are valuable tools for the study of star formation in the Å wavelength intervals at spectral resolution of ~700, from early Universe. High redshift quasars are bright, and thus easily which spectra of the different sources will be retrieved. A 5s observable objects, ideally located in redshift to probe their host depth of 10-18 erg/cm2/s will make OTELO the deepest emission galaxies’ metallicities at great distances and early times. Their line survey to date. The expected number of emitters is of the location within the host galaxy allows these metallicity measure- order of 10000, where 10% would be Ha star forming emitters ments to be made through observing the quasar emission and up to a z= 0.4 (about 10% of these would be low luminosity star absorption lines. Most of the work so far has used the emission forming galaxies), 70% would be star forming emitters detected lines, as they are relatively easy to measure in large samples of at other optical emission lines up to a z = 1.5; 5% Lya emitters at objects. The results suggest that quasar environments are typi- z up to 6.7 (10% of the age of the Universe), 15% QSO and AGNs cally metal rich, with gas-phase metallicities near solar or higher 49 at all observed redshifts. However this analysis has some signifi- P61 cant uncertainties. Other independent abundance checks are GOYA SURVEY: U, B and K Galaxy Number Counts needed in order to confirm results from this popular technique. Mercedes Prieto; M.Carmen Eliche-Moral; Marc Balcells; Cesar We use very high resolution echelle spectra from VLT-UVES for E. Garcia-Dabo; Peter Erwin; David Cristobal-Hornillos 8 high redshift (z of 2 to z of 4.6) quasars, selected to contain Instituto de Astrofisica de Canarias candidate intrinsic absorbers, and encompassing a typical rest- frame spectral range from approximately 900 Angstroms to 2500 We present U and B number counts from a field of the GOYA Angstroms, designed to include at least Lyman alpha and CIV Survey that covers ~900 sq. arcmin over the Groth-Westphal spectral features. We perform one of the first analyses of absorp- Strip. Achieved limiting magnitudes (50% detection efficiency tion line metallicities in high redshift quasars and present first es- for point sources) are U = 24.8 mag and B = 25.5 mag, in the timates of these metallicites as well as estimates for the absorber Vega system. The counts have been corrected for detection ef- locations relative to the quasar. This new information will shed ficiency as a function of source size, for spurious detections and more light on the star formation in these high redshift objects, star-galaxy separation. with high metallicities supporting earlier suggestions of multiple epochs of star formation at early times. The GTC will be impor- Counts are given over 18.0

P60 Bulge colors of intermediate redshift galaxies L. Dominguez-Palmero; M. Balcells; M. Prieto Instituto de Astrofisica de Canarias We have studied the colors of the bulge component of 123 gal- axies from the HST Groth Strip Survey, covering redshifts 0.1 < z < 1.3. We selected all objects with apparent radii R > 1.4’’, P62 and with inclination above 50° in order to avoid reddening from High Velocity Outflows in Quasars dust in the disk on one side of the bulges. We find that, as in the Local Universe, the minor axis color profiles are negative (bluer Paola Rodriguez Hidalgo; Fred Hamann; Daniel Nestor outward), and fairly gentle, indicating that bulge colors are not University of Florida distinctly different from disk colors. In most cases, dust bands are Active Galactic Nuclei (AGN) are believed to be powered by the most important morphological structure in the color maps. accretion onto a Super-Massive Black Holes (SMBH). In order to In a subsample of big-bulge galaxies, we analize central rest- have material falling into the SMBH, angular momentum con- frame colors using K-corrections. Bulge colors do not globally servation requires a counterpart for this accretion that is fueling become bluer at higher redshifts. This suggests that there were the SMBH in the AGN. Outflows might play an essential role ``old’’ bulges at z = 0.8’’. The color-magnitude distribution of in active galactic nuclei. They show common occurance, both intermediate-z bulges shows more color dispersion than that of in quasars (30%-40% in optically selected quasars) and Seyfert bulges in the Local Universe. About 50% of bulges are as red as galaxies (approx. 60%), but might be obiquitous if, they only sub- local bulges, while the remainder are significantly bluer, a pos- tend a small angular distance in the sky. Moreover, they bring sible sign of late bulge formation. information from the AGN inner regions, which is not accesible through other ways. Notes: Although for more than a decade models have included material outflowing from an accretion disk around a SMBH, surprisingly there is no consensus in our understanding of basic properties like the acceleration mechanism(s), launch radii, mass loss rates, terminal velocities, etc. We are involved in a program to derive basic dynamical characteristics for some well-studied individual flows. Moreover, we are especially interested in High Velocity (HV) outflows since they will present unique challenges for the above mentioned theoretical models. Previously some classes of outflows have been studied, such as 50 the broad absorption lines (BALs; FWHM > 3,000 km/s). We Notes: have developed the first systematic accounting of outflow lines, taking advantage of Sloan Digital Sky Survey data. Based on this work, we have begun a program to study a nearly unexplored part of AGN parameter space: HV winds with v > 10,000 km/s but small velocity dispersions (narrow absorption lines), previ- ously attributed to unrelated (intervening) gas, but that recent statistical studies confirm to be (approx. 36%) AGN winds. Vari- ability studies can confirm whether absorption lines are unrelat- ed (intervening) or related to the AGN (winds). We are currently collecting data on this matter. The GTC will allow us to extend this work into the larger context of AGN/SMBH/galaxy evolution. For example, deep red and in- P65 frared spectroscopy and adaptive optics imaging will allow us to Elmer Imaging: Characterization and Perfor- push to higher redshifts, to fainter and less massive objects, and mance results from the Pre-shipping Acceptance examine the relationship of AGN accretion/wind properties to Tests the host galaxy environments. Juanma Martin-Fleitas; Maria L. García-Vargas; Antonio Ca- Notes: brera Lavers; Ralf Kohley; Peter Hammersley; Ernesto Sanchez- Blanco; Manuel Maldonado IAC Elmer is a multi-purpose instrument for the GTC designed for both, Imaging and Spectroscopy in the visible range (365nm - 1000 nm). Elmer has been exhaustively characterized at la La- guna for 2 years. Imaging will be done through standard SDSS broad band filters as well as a set of narrow band filters. This poster presents the instrument performance in terms of FOV, fiducial position, plate scale, field distortion, flexures, focus, image quality, throughput, P63 ghosts, stray light control, etc as well as a detailed discussion for Active Galactic Nuclei Surveys with the GTC Narrow Band Imaging with real data. Vicki Sarajedini Finally, we summary the results and performance at laboratory University of Florida for the fast spectro-photometry modes. This opens a wide range Active Galactic Nuclei candidates can be identified in deep, of scientific possibilities for time-resolved observations. This can multi wave length surveys via an array of selection techniques. be done thanks to the design of this mode from the beginning This talk will discuss recent surveys for AGN in deep HST fields and the use of an E2V Technologies CCD44-82 detector with and the use of the GTC and, more specifically, the GOYA project Frame Transfer and Charge Shuffling capabilities. to investigate the AGN population at z=1. Notes: Notes:

P66 P64 Elmer Spectroscopy: Characterization and Per- Multiwavelength analysis of H alpha selected formance results from the Pre-shipping Accep- galaxies at z=0.6 tance Tests Villar, V.; Gallego, J.; Zamorano, J.; Koo, D; Noeske, K Antonio Cabrera Lavers; Juanma Martin-Fleitas; Maria L. Gar- Universidad Complutense de Madrid cía-Vargas; Peter Hammersley; Ralf Kohley; Ernesto Sanchez- Blanco; Manuel Maldonado We present an Ha-selected galaxy sample at z~0.8. Objects have IAC been selected by their contrast in narrow band filters centered at 12000Å and its nature has been confirmed with optical spectros- Elmer is a multi-purpose instrument for the GTC designed for copy. Ha luminosity function and Star Formation Rate density both, Imaging and Spectroscopy, in the visible range (365nm (SFRd) have been measu red and presented. A multiwavelength - 1000 nm). Elmer has been exhaustively characterized at la La- analysis has been carried out in order to compare the different guna for 2 years. Spectroscopy is done with prisms, grisms and star formation rates obtained with the UV continuum, [OII] line VPHs, providing resolution powers of 200, 1000 and 2500 over flux, Ha line flux and IR flux. the whole wavelength range. 51 The complete set of tests has allowed characterizing important parameters like: fiducial position and slit viewing (for acquisi- tion), spectral coverage, spectral resolution (Resolving Power, Dispersion), central wavelength, flexures, focus, image quality, throughput and ghosts, associated to each of the dispersive el- ements and in each of the possible configurations. This poster summarizes the performance in both, Long Slit and Multi-object modes, as well as provides a summary of the calibration and data reduction strategies for Spectroscopy with Elmer. Notes:

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