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Near-Infrared Luminosity Relations and Dust Colors L
A&A 578, A47 (2015) Astronomy DOI: 10.1051/0004-6361/201525817 & c ESO 2015 Astrophysics Obscuration in active galactic nuclei: near-infrared luminosity relations and dust colors L. Burtscher1, G. Orban de Xivry1, R. I. Davies1, A. Janssen1, D. Lutz1, D. Rosario1, A. Contursi1, R. Genzel1, J. Graciá-Carpio1, M.-Y. Lin1, A. Schnorr-Müller1, A. Sternberg2, E. Sturm1, and L. Tacconi1 1 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Gießenbachstr., 85741 Garching, Germany e-mail: [email protected] 2 Raymond and Beverly Sackler School of Physics & Astronomy, Tel Aviv University, 69978 Ramat Aviv, Israel Received 5 February 2015 / Accepted 5 April 2015 ABSTRACT We combine two approaches to isolate the AGN luminosity at near-IR wavelengths and relate the near-IR pure AGN luminosity to other tracers of the AGN. Using integral-field spectroscopic data of an archival sample of 51 local AGNs, we estimate the fraction of non-stellar light by comparing the nuclear equivalent width of the stellar 2.3 µm CO absorption feature with the intrinsic value for each galaxy. We compare this fraction to that derived from a spectral decomposition of the integrated light in the central arcsecond and find them to be consistent with each other. Using our estimates of the near-IR AGN light, we find a strong correlation with presumably isotropic AGN tracers. We show that a significant offset exists between type 1 and type 2 sources in the sense that type 1 MIR X sources are 7 (10) times brighter in the near-IR at log LAGN = 42.5 (log LAGN = 42.5). -
On the Origin and Propagation of Ultra-High Energy Cosmic Rays (Measurements & Prediction Techniques)
Dissertation On the Origin and Propagation of Ultra-High Energy Cosmic Rays (Measurements & Prediction Techniques) Nils Nierstenhoefer Wuppertal, 2011 University of Wuppertal Supervisor/First reviewer: Prof. Dr. K.-H. Kampert Second reviewer: Prof. Dr. M. Risse Motivation & Preface It is a long known fact that cosmic rays reach Earth with tremendous energies of even above 1020 eV. Despite of decades of intensive research, it was not possible to finally reveal the origin of these par- ticles. The main obstacle in this field is their rare occurrence. This is due to a very steep energy spectrum. To make this point more clear, one roughly expects to observe less than one particle per km2 in one century exceeding energies larger than 1020 eV. To overcome the limitation of low statis- tics, larger and larger cosmic ray detectors have been deployed. Today’s largest cosmic ray detector is the Pierre Auger observatory (PAO) which was constructed in the Pampa Amarilla in Argentina. It covers an area of 3000 km2 and provides the largest set of observations of ultra-high energy cosmic rays (UHECR) in history. A second difficulty in understanding the origin of UHECR should be pointed out: Galactic and extra- galactic magnetic fields might alter the direction of even the highest energy events in a way that they do not point back to their source. In 2007 and 2008, already before the completion of the full detector, the Auger collaboration pub- lished a set of three important papers [1, 2, 3]. The first paper dealt with the correlation of the arrival directions of the highest energetic events with the distribution of active galactic nuclei (AGN) closer than 75Mpc from a catalog compiled by Veron-Cetty and Veron (VC-V) [4]. -
April Constellations of the Month
April Constellations of the Month Leo Small Scope Objects: Name R.A. Decl. Details M65! A large, bright Sa/Sb spiral galaxy. 7.8 x 1.6 arc minutes, magnitude 10.2. Very 11hr 18.9m +13° 05’ (NGC 3623) high surface brighness showing good detail in medium sized ‘scopes. M66! Another bright Sb galaxy, only 21 arc minutes from M65. Slightly brighter at mag. 11hr 20.2m +12° 59’ (NGC 3627) 9.7, measuring 8.0 x 2.5 arc minutes. M95 An easy SBb barred spiral, 4 x 3 arc minutes in size. Magnitude 10.5, with 10hr 44.0m +11° 42’ a bright central core. The bar and outer ring of material will require larger (NGC 3351) aperature and dark skies. M96 Another bright Sb spiral, about 42 arc minutes east of M95, but larger and 10hr 46.8m +11° 49’ (NGC 3368) brighter. 6 x 4 arc minutes, magnitude 10.1. Located about 48 arc minutes NNE of M96. This small elliptical galaxy measures M105 only 2 x 2.1 arc minutes, but at mag. 10.3 has very high surface brightness. 10hr 47.8m +12° 35’ (NGC 3379) Look for NGC 3384! (110NGC) and NGC 3389 (mag 11.0 and 12.2) which form a small triangle with M105. NGC 3384! 10hr 48.3m +12° 38’ See comment for M105. The brightest galaxy in Leo, this Sb/Sc spiral galaxy shines at mag. 9.5. Look for NGC 2903!! 09hr 32.2m +21° 30’ a hazy patch 11 x 4.7 arc minutes in size 1.5° south of l Leonis. -
Nicholas Stone Einstein Fellow, Columbia University MODEST-18 6/29/18
Elevated Tidal Disruption Rates in Post-Starburst Galaxies Nicholas Stone Einstein Fellow, Columbia University MODEST-18 6/29/18 With: Aleksey Generozov, Eugene Vasiliev, Brian Metzger, Sjoert van Velzen A View to a Kill MBH=106M⦿, aBH=0.9, i=90˚ Face-On Edge-On Rt Rt PN-SPH (Hayasaki, NCS & Loeb 16) He IIλ4686 line is still evident as an excess above the model in the later epoch, however it has faded by a factor of ∼ 10 since the pre-preak spectrum, the same factor by which the ultraviolet continuum has faded during this time. Note that the absolute flux scaling in the later epoch is uncertain due to clouds on the date of the observation. Tidal Disruption Events • Empirically: ✦ Rare multiwavelength (radio -> hard X-ray) transients ✦ Dozens of strong candidate flares (most optical/X-ray) • Applications: Figure 2 ✦ Ultraviolet and optical light curve. The GALEX NUV and PS1 gP1-, rP1-, iP1-, and zP1- Tools to measure SMBH demographyband light curve of PS1-10jh (with the host galaxy flux removed) with 1σ error bars and in logarithmic days since the time of disruption determined from the best fit of the rP1-band (mass, maybe spin) light curve to the numerical model20 for the mass accretion rate of a tidally disrupted star with a polytropic exponent of 5/3 (shown with solid lines scaled to the flux in the GALEX and PS1 bands). The GALEX and PS1 photometry at t>240 rest-frame days since ✦ Super-Eddington accretion the peak is shown binned in time in order to increase the signal-to-noise. -
A Disturbed Galactic Duo 20 April 2011
A disturbed galactic duo 20 April 2011 neighbours. This galactic grouping, found about 70 million light- years away in the constellation Sextans (The Sextant), was discovered by the English astronomer William Herschel in 1783. Modern astronomers have gauged the distance between NGC 3169 (left) and NGC 3166 (right) as a mere 50 000 light-years, a separation that is only about half the diameter of the Milky Way galaxy. In such tight quarters, gravity can start to play havoc with galactic structure. Spiral galaxies like NGC 3169 and NGC 3166 tend to have orderly swirls of stars and dust pinwheeling about their glowing centres. Close encounters with other massive objects can jumble this classic configuration, often serving as a disfiguring prelude to the merging of galaxies into one larger galaxy. So far, the interactions of NGC 3169 and NGC 3166 have just lent a bit of character. NGC 3169's This image from the Wide Field Imager on the arms, shining bright with big, young, blue stars, MPG/ESO 2.2-meter telescope at the La Silla have been teased apart, and lots of luminous gas Observatory in Chile captures the pair of galaxies NGC has been drawn out from its disc. In NGC 3166's 3169 (left) and NGC 3166 (right). These adjacent case, the dust lanes that also usually outline spiral galaxies display some curious features, demonstrating arms are in disarray. Unlike its bluer counterpart, that each member of the duo is close enough to feel the NGC 3166 is not forming many new stars. distorting gravitational influence of the other. -
TSP 2004 Telescope Observing Program
THE TEXAS STAR PARTY 2004 TELESCOPE OBSERVING CLUB BY JOHN WAGONER TEXAS ASTRONOMICAL SOCIETY OF DALLAS RULES AND REGULATIONS Welcome to the Texas Star Party's Telescope Observing Club. The purpose of this club is not to test your observing skills by throwing the toughest objects at you that are hard to see under any conditions, but to give you an opportunity to observe 25 showcase objects under the ideal conditions of these pristine West Texas skies, thus displaying them to their best advantage. This year we have planned a program called “Starlight, Starbright”. The rules are simple. Just observe the 25 objects listed. That's it. Any size telescope can be used. All observations must be made at the Texas Star Party to qualify. All objects are within range of small (6”) to medium sized (10”) telescopes, and are available for observation between 10:00PM and 3:00AM any time during the TSP. Each person completing this list will receive an official Texas Star Party Telescope Observing Club lapel pin. These pins are not sold at the TSP and can only be acquired by completing the program, so wear them proudly. To receive your pin, turn in your observations to John Wagoner - TSP Observing Chairman any time during the Texas Star Party. I will be at the outside door leading into the TSP Meeting Hall each day between 1:00 PM and 2:30 PM. If you finish the list the last night of TSP, or I am not available to give you your pin, just mail your observations to me at 1409 Sequoia Dr., Plano, Tx. -
April 14 2018 7:00Pm at the April 2018 Herrett Center for Arts & Science College of Southern Idaho
Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Tim Frazier Saturday, April 14th 2018 April 2018 7:00pm at the Herrett Center for Arts & Science College of Southern Idaho. It really is beginning to feel like spring. The weather is more moderate and there will be, hopefully, clearer skies. (I write this with some trepidation as I don’t want to jinx Public Star Party Follows at the it in a manner similar to buying new equipment will ensure at least two weeks of Centennial Observatory cloudy weather.) Along with the season comes some great spring viewing. Leo is high overhead in the early evening with its compliment of galaxies as is Coma Club Officers Berenices and Virgo with that dense cluster of extragalactic objects. Tim Frazier, President One of my first forays into the Coma-Virgo cluster was in the early 1960’s with my [email protected] new 4 ¼ inch f/10 reflector and my first star chart, the epoch 1960 version of Norton’s Star Atlas. I figured from the maps I couldn’t miss seeing something since Robert Mayer, Vice President there were so many so closely packed. That became the real problem as they all [email protected] appeared as fuzzy spots and the maps were not detailed enough to distinguish one galaxy from another. I still have that atlas as it was a precious Christmas gift from Gary Leavitt, Secretary my grandparents but now I use better maps, larger scopes and GOTO to make sure [email protected] it is M84 or M86. -
Arxiv:2105.08061V1 [Astro-Ph.GA] 17 May 2021
Draft version May 19, 2021 Typeset using LATEX twocolumn style in AASTeX63 A recently quenched isolated dwarf galaxy outside of the Local Group environment Ava Polzin,1 Pieter van Dokkum,1 Shany Danieli,1, 2, 3, 4, ∗ Johnny P. Greco,5, y and Aaron J. Romanowsky6, 7 1Department of Astronomy, Yale University, New Haven, CT 06511, USA 2Department of Physics, Yale University, New Haven, CT 06520, USA 3Yale Center for Astronomy and Astrophysics, Yale University, New Haven, CT 06511, USA 4Institute for Advanced Study, 1 Einstein Drive, Princeton, NJ 08540, USA 5Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, Columbus, OH 43210, USA 6Department of Physics & Astronomy, One Washington Square, San Jos´eState University, San Jose, CA 95192, USA 7University of California Observatories, 1156 High Street, Santa Cruz, CA 95064, USA (Received March 22, 2021; Revised May 14, 2021; Accepted May 17, 2021) Submitted to ApJL ABSTRACT 6 We report the serendipitous identification of a low mass (M∗ ∼ 2×10 M ), isolated, likely quenched dwarf galaxy in the \foreground" of the COSMOS-CANDELS field. From deep Hubble Space Telescope (HST) imaging we infer a surface brightness fluctuation distance for COSMOS-dw1 of DSBF = 22 ± 3 Mpc, which is consistent with its radial velocity of cz = 1222 ± 64 km s−1 via Keck/LRIS. At this distance, the galaxy is 1.4 Mpc in projection from its nearest massive neighbor. We do not detect significant Hα emission (EW(Hα)= −0:4 ± 0:5 A),˚ suggesting that COSMOS-dw1 is likely quenched. Very little is currently known about isolated quenched galaxies in this mass regime. -
SAC's 110 Best of the NGC
SAC's 110 Best of the NGC by Paul Dickson Version: 1.4 | March 26, 1997 Copyright °c 1996, by Paul Dickson. All rights reserved If you purchased this book from Paul Dickson directly, please ignore this form. I already have most of this information. Why Should You Register This Book? Please register your copy of this book. I have done two book, SAC's 110 Best of the NGC and the Messier Logbook. In the works for late 1997 is a four volume set for the Herschel 400. q I am a beginner and I bought this book to get start with deep-sky observing. q I am an intermediate observer. I bought this book to observe these objects again. q I am an advance observer. I bought this book to add to my collect and/or re-observe these objects again. The book I'm registering is: q SAC's 110 Best of the NGC q Messier Logbook q I would like to purchase a copy of Herschel 400 book when it becomes available. Club Name: __________________________________________ Your Name: __________________________________________ Address: ____________________________________________ City: __________________ State: ____ Zip Code: _________ Mail this to: or E-mail it to: Paul Dickson 7714 N 36th Ave [email protected] Phoenix, AZ 85051-6401 After Observing the Messier Catalog, Try this Observing List: SAC's 110 Best of the NGC [email protected] http://www.seds.org/pub/info/newsletters/sacnews/html/sac.110.best.ngc.html SAC's 110 Best of the NGC is an observing list of some of the best objects after those in the Messier Catalog. -
Arxiv:Astro-Ph/0310277V1 9 Oct 2003 Tdb H Soito Fuieste O Eerhi Astr in Foundation
The Globular Cluster Systems of the Early-type Galaxies NGC 3379, NGC 4406, and NGC 4594 and Implications for Galaxy Formation Katherine L. Rhode1,2 Department of Astronomy, Yale University, New Haven, CT 06520 [email protected] Stephen E. Zepf1 Department of Physics & Astronomy, Michigan State University, East Lansing, MI 48824 [email protected] ABSTRACT We have investigated the global properties of the globular cluster (GC) systems of three early-type galaxies: the Virgo cluster elliptical NGC 4406, the field elliptical NGC 3379, and the field S0 galaxy NGC 4594. These galaxies were observed as part of a wide-field CCD survey of the GC populations of a large sample of normal galaxies beyond the Local Group. Images obtained with the Mosaic detector on the Kitt Peak 4-m telescope provide radial coverage to at least 24′, or ∼70−100 kpc. We use BV R photometry and image classification to select GC candidates and thereby reduce con- tamination from non-GCs, and HST WFPC2 data to help quantify the contamination that remains. The GC systems of all three galaxies have color distributions with at least two peaks and show modest negative color gradients. The proportions of blue GCs range from 60−70% of the total populations. The GC specific frequency (SN ) of arXiv:astro-ph/0310277v1 9 Oct 2003 NGC 4406 is 3.5±0.5, ∼20% lower than past estimates and nearly identical to SN for the other Virgo cluster elliptical included in our survey, NGC 4472. SN for NGC 3379 and NGC 4594 are 1.2±0.3 and 2.1±0.3, respectively; these are similar to past values but the errors have been reduced by a factor of 2−3. -
SAA 100 Club
S.A.A. 100 Observing Club Raleigh Astronomy Club Version 1.2 07-AUG-2005 Introduction Welcome to the S.A.A. 100 Observing Club! This list started on the USENET newsgroup sci.astro.amateur when someone asked about everyone’s favorite, non-Messier objects for medium sized telescopes (8-12”). The members of the group nominated objects and voted for their favorites. The top 100 objects, by number of votes, were collected and ranked into a list that was published. This list is a good next step for someone who has observed all the objects on the Messier list. Since it includes objects in both the Northern and Southern Hemispheres (DEC +72 to -72), the award has two different levels to accommodate those observers who aren't able to travel. The first level, the Silver SAA 100 award requires 88 objects (all visible from North Carolina). The Gold SAA 100 Award requires all 100 objects to be observed. One further note, many of these objects are on other observing lists, especially Patrick Moore's Caldwell list. For convenience, there is a table mapping various SAA100 objects with their Caldwell counterparts. This will facilitate observers who are working or have worked on these lists of objects. We hope you enjoy looking at all the great objects recommended by other avid astronomers! Rules In order to earn the Silver certificate for the program, the applicant must meet the following qualifications: 1. Be a member in good standing of the Raleigh Astronomy Club. 2. Observe 80 Silver observations. 3. Record the time and date of each observation. -
Aaron J. Romanowsky Curriculum Vitae (Rev. 1 Septembert 2021) Contact Information: Department of Physics & Astronomy San
Aaron J. Romanowsky Curriculum Vitae (Rev. 1 Septembert 2021) Contact information: Department of Physics & Astronomy +1-408-924-5225 (office) San Jose´ State University +1-409-924-2917 (FAX) One Washington Square [email protected] San Jose, CA 95192 U.S.A. http://www.sjsu.edu/people/aaron.romanowsky/ University of California Observatories +1-831-459-3840 (office) 1156 High Street +1-831-426-3115 (FAX) Santa Cruz, CA 95064 [email protected] U.S.A. http://www.ucolick.org/%7Eromanow/ Main research interests: galaxy formation and dynamics – dark matter – star clusters Education: Ph.D. Astronomy, Harvard University Nov. 1999 supervisor: Christopher Kochanek, “The Structure and Dynamics of Galaxies” M.A. Astronomy, Harvard University June 1996 B.S. Physics with High Honors, June 1994 College of Creative Studies, University of California, Santa Barbara Employment: Professor, Department of Physics & Astronomy, Aug. 2020 – present San Jose´ State University Associate Professor, Department of Physics & Astronomy, Aug. 2016 – Aug. 2020 San Jose´ State University Assistant Professor, Department of Physics & Astronomy, Aug. 2012 – Aug. 2016 San Jose´ State University Research Associate, University of California Observatories, Santa Cruz Oct. 2012 – present Associate Specialist, University of California Observatories, Santa Cruz July 2007 – Sep. 2012 Researcher in Astronomy, Department of Physics, Oct. 2004 – June 2007 University of Concepcion´ Visiting Adjunct Professor, Faculty of Astronomical and May 2005 Geophysical Sciences, National University of La Plata Postdoctoral Research Fellow, School of Physics and Astronomy, June 2002 – Oct. 2004 University of Nottingham Postdoctoral Fellow, Kapteyn Astronomical Institute, Oct. 1999 – May 2002 Rijksuniversiteit Groningen Research Fellow, Harvard-Smithsonian Center for Astrophysics June 1994 – Oct.