SMBH Mass Estimation in NGC 1097 ALMA
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Radio Continuum and CO Emission in Star-Forming Galaxies
A&A 385, 412–424 (2002) Astronomy DOI: 10.1051/0004-6361:20020140 & c ESO 2002 Astrophysics Radio continuum and CO emission in star-forming galaxies M. Murgia1,A.Crapsi1,2, L. Moscadelli3, and L. Gregorini1,4 1 Istituto di Radioastronomia del CNR, Via Gobetti 101, 40129, Bologna, Italy 2 Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Firenze, Italy 3 Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54, 09012 Capoterra (CA), Italy 4 Dipartimento di Fisica, Universit`a di Bologna, Via B. Pichat 6/2, 40127 Bologna, Italy Received 30 October 2001 / Accepted 23 January 2002 Abstract. We combine the radio continuum images from the NRAO VLA Sky Survey with the CO-line observations from the extragalactic CO survey of the Five College Radio Astronomy Observatory to study the relationship between molecular gas and the star formation rate within the disks of 180 spiral galaxies at 4500 resolution. We find a tight correlation between these quantities. On average, the ratio between the radio continuum and the CO emission is constant, within a factor of 3, both inside the same galaxy and from galaxy to galaxy. The mean star formation efficiency deduced from the radio continuum corresponds to convert 3.5% of the available molecular gas into stars on a time scale of 108 yr and depends weakly on general galaxy properties, such as Hubble type or nuclear activity. A comparison is made with another similar analysis performed using the Hα luminosity as star formation indicator. The overall agreement we find between the two studies reinforces the use of the radio luminosity as star formation rate indicator not only on global but also on local scales. -
The Centre of the Active Galaxy NGC 1097
Figure 4: Relative map- References ping speed of SCOWL 1000000 versus the ALMA Com- The OWL Instrument Concept Studies have been pact Configuration. published as ESO internal reports. They can be ob- tained from the PI’s or ESO. 10000 (1) D’Odorico S., Moorwood A. F .M., Beckers, J. 1991, Journal of Optics 22, 85 (2) CODEX, Cosmic Dynamics Experiment, OWL–CSR-ESO-00000-0160, October 2005 100 (3) T-OWL, Thermal Infrared Imager and Spectrograph for OWL, OWL–CSR-ESO-00000-0161, October 2005 (4) QuantEYE, OWL–CSR-ESO-00000-0162, October 0 2005 (5) SCOWL, Submillimeter Camera for OWL; OWL–CSR-ESO-00000-0163, September 2005 (6) MOMFIS, Multi Object Multi Field IR Spectrograph, OWL–CSR-ESO-00000-0164, September 2005 0.01 (7) ONIRICA, OWL NIR Imaging Camera, OWL–CSR-ESO-00000-0165, October 2005 (8) EPICS, Earth-like Planet Imaging Camera and Spectrograph, OWL–CSR-ESO-00000-0166, 0.0001 October 2005 850 450 350 850 450 350 λ(µm) (9) HyTNIC, Hyper-Telescope Near Infrared Camera, ALMA Compact SCOWL OWL–CSR-ESO-00000-0167, October 2005 The Centre of the Active Galaxy NGC 1097 Near-infrared images of the active galaxy A colour-composite image of the cen- NGC 1097 have been obtained by a team of tral 5 500 light-years wide region of astronomers1 using NACO on the VLT. Located the spiral galaxy NGC 1097, obtained with NACO on the VLT. More than at a distance of about 45 million light years in 300 star-forming regions – white spots the southern constellation Fornax, NGC 1097 is in the image – are distributed along a relatively bright, barred spiral galaxy seen a ring of dust and gas in the image. -
Chemistry and Star Formation in the Host Galaxies of Type Ia Supernovae
Chemistry and Star Formation in the Host Galaxies of Type Ia Supernovae The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Gallagher, Joseph S., Peter M. Garnavich, Perry Berlind, Peter Challis, Saurabh Jha, and Robert P. Kirshner. 2005. “Chemistry and Star Formation in the Host Galaxies of Type Ia Supernovae.” The Astrophysical Journal 634 (1): 210–26. https:// doi.org/10.1086/491664. Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:41399918 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Other Posted Material, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#LAA The Astrophysical Journal, 634:210–226, 2005 November 20 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. CHEMISTRY AND STAR FORMATION IN THE HOST GALAXIES OF TYPE Ia SUPERNOVAE Joseph S. Gallagher and Peter M. Garnavich Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556-5670 Perry Berlind F. L. Whipple Observatory, 670 Mount Hopkins Road, P.O. Box 97, Amado, AZ 85645 Peter Challis Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Saurabh Jha Department of Astronomy, 601 Campbell Hall, University of California, Berkeley, CA 94720-3411 and Robert P. Kirshner Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Received 2005 March 4; accepted 2005 July 22 ABSTRACT We study the effect of environment on the properties of Type Ia supernovae by analyzing the integrated spectra of 57 local Type Ia supernova host galaxies. -
Pdf, Dry Merger Rate and Post-Merger Fraction in the Coma Cluster Core
The Astrophysical Journal Letters, 817:L6 (7pp), 2016 January 20 doi:10.3847/2041-8205/817/1/L6 © 2016. The American Astronomical Society. All rights reserved. DRY MERGER RATE AND POST-MERGER FRACTION IN THE COMA CLUSTER CORE Juan P. Cordero1, Luis E. Campusano1, Roberto De Propris2, Christopher P. Haines1, Tim Weinzirl3, and Shardha Jogee4 1 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile; [email protected] 2 Finnish Centre for Astronomy with ESO, University of Turku, Vaisalantie 20, Piikkio, FI-21500, Finland 3 School of Physics and Astronomy, The University of Nottingham, University Park, Nottingham NG7 2RD, UK 4 Department of Astronomy, The University of Texas at Austin, Austin, TX 78712-1205, USA Received 2015 August 27; accepted 2015 December 21; published 2016 January 19 ABSTRACT We evaluate the dry merger activity in the Coma cluster, using a spectroscopically complete sample of 70 red- sequence (RS) galaxies, most of which (∼75%) are located within 0.2R200 (∼0.5 Mpc) from the cluster center, with data from the Coma Treasury Survey obtained with the Hubble Space Telescope. The fraction of close galaxy pairs in the sample is the proxy employed for the estimation of the merger activity. We identify 5 pairs and 1 triplet, enclosing a total of 13 galaxies, based on limits on projected separation and line-of-sight velocity difference. Of these systems, none show signs of ongoing interaction, and therefore we do not find any true mergers in our sample. This negative result sets a 1σ upper limit of 1.5% per Gyr for the major dry merger rate, consistent with the low rates expected in present-day clusters. -
The Dynamical State of the Coma Cluster with XMM-Newton?
A&A 400, 811–821 (2003) Astronomy DOI: 10.1051/0004-6361:20021911 & c ESO 2003 Astrophysics The dynamical state of the Coma cluster with XMM-Newton? D. M. Neumann1,D.H.Lumb2,G.W.Pratt1, and U. G. Briel3 1 CEA/DSM/DAPNIA Saclay, Service d’Astrophysique, L’Orme des Merisiers, Bˆat. 709, 91191 Gif-sur-Yvette, France 2 Science Payloads Technology Division, Research and Science Support Dept., ESTEC, Postbus 299 Keplerlaan 1, 2200AG Noordwijk, The Netherlands 3 Max-Planck Institut f¨ur extraterrestrische Physik, Giessenbachstr., 85740 Garching, Germany Received 19 June 2002 / Accepted 13 December 2002 Abstract. We present in this paper a substructure and spectroimaging study of the Coma cluster of galaxies based on XMM- Newton data. XMM-Newton performed a mosaic of observations of Coma to ensure a large coverage of the cluster. We add the different pointings together and fit elliptical beta-models to the data. We subtract the cluster models from the data and look for residuals, which can be interpreted as substructure. We find several significant structures: the well-known subgroup connected to NGC 4839 in the South-West of the cluster, and another substructure located between NGC 4839 and the centre of the Coma cluster. Constructing a hardness ratio image, which can be used as a temperature map, we see that in front of this new structure the temperature is significantly increased (higher or equal 10 keV). We interpret this temperature enhancement as the result of heating as this structure falls onto the Coma cluster. We furthermore reconfirm the filament-like structure South-East of the cluster centre. -
Virgo the Virgin
Virgo the Virgin Virgo is one of the constellations of the zodiac, the group tion Virgo itself. There is also the connection here with of 12 constellations that lies on the ecliptic plane defined “The Scales of Justice” and the sign Libra which lies next by the planets orbital orientation around the Sun. Virgo is to Virgo in the Zodiac. The study of astronomy had a one of the original 48 constellations charted by Ptolemy. practical “time keeping” aspect in the cultures of ancient It is the largest constellation of the Zodiac and the sec- history and as the stars of Virgo appeared before sunrise ond - largest constellation after Hydra. Virgo is bordered by late in the northern summer, many cultures linked this the constellations of Bootes, Coma Berenices, Leo, Crater, asterism with crops, harvest and fecundity. Corvus, Hydra, Libra and Serpens Caput. The constella- tion of Virgo is highly populated with galaxies and there Virgo is usually depicted with angel - like wings, with an are several galaxy clusters located within its boundaries, ear of wheat in her left hand, marked by the bright star each of which is home to hundreds or even thousands of Spica, which is Latin for “ear of grain”, and a tall blade of galaxies. The accepted abbreviation when enumerating grass, or a palm frond, in her right hand. Spica will be objects within the constellation is Vir, the genitive form is important for us in navigating Virgo in the modern night Virginis and meteor showers that appear to originate from sky. Spica was most likely the star that helped the Greek Virgo are called Virginids. -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
Spatially Resolved Spectroscopy of Coma Cluster Early–Type Galaxies
ASTRONOMY & ASTROPHYSICS FEBRUARY I 2000, PAGE 449 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 141, 449–468 (2000) Spatially resolved spectroscopy of Coma cluster early–type galaxies I. The database ? D. Mehlert1,2,??,???,????, R.P. Saglia1,R.Bender1,andG.Wegner3 1 Universit¨atssternwarte M¨unchen, 81679 M¨unchen, Germany 2 Present address: Landessternwarte Heidelberg, 69117 Heidelberg, Germany 3 Department of Physics and Astronomy, 6127 Wilder Laboratory, Dartmouth College, Hanover, NH 03755-3528, U.S.A. Received March 8; accepted September 30, 1999 Abstract. We present long slit spectra for a magnitude Key words: galaxies: elliptical and lenticular, cD; limited sample of 35 E and S0 galaxies of the Coma cluster. kinematics and dynamics; stellar content; abundances; The high quality of the data allowed us to derive spatially formation resolved spectra for a substantial sample of Coma galaxies for the first time. From these spectra we obtained rota- tion curves, the velocity dispersion profiles and the H3 and H4 coefficients of the Hermite decomposition of the 1. Introduction line of sight velocity distribution. Moreover, we derive the radial line index profiles of Mg, Fe and Hβ line indices This is the first of a series of papers aiming at investi- out to R ≈ 1re − 3re with high signal-to-noise ratio. We gating the stellar populations, the radial distribution and describe the galaxy sample, the observations and data re- the dynamics of early-type galaxies as a function of the duction, and present the spectroscopic database. Ground- environmental density. Spanning about 4 decades in den- based photometry for a subsample of 8 galaxies is also sity, the Coma cluster is the ideal place to perform such a presented. -
May 2013 BRAS Newsletter
www.brastro.org May 2013 What's in this issue: PRESIDENT'S MESSAGE .............................................................................................................................. 2 NOTES FROM THE VICE PRESIDENT ........................................................................................................... 3 MESSAGE FROM THE HRPO ...................................................................................................................... 4 OBSERVING NOTES ..................................................................................................................................... 5 DEEP SKY OBJECTS ................................................................................................................................... 6 MAY ASTRONOMICAL EVENTS .................................................................................................................... 7 TREASURER’S NOTES ................................................................................................................................. 8 PREVIOUS MEETING MINUTES .................................................................................................................... 9 IMPORTANT NOTE: This month's meeting will be held on Saturday, May 18th at LIGO. PRESIDENT'S MESSAGE Hi Everyone, April was quite a busy month and the busiest day was International Astronomy Day. As you may have heard, we had the highest attendance at our Astronomy Day festivities at the HRPO ever. Approximately 770 people attended this year -
University of Groningen the Galaxy Population in the Coma Cluster Beijersbergen, Marco
University of Groningen The galaxy population in the Coma cluster Beijersbergen, Marco IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2003 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Beijersbergen, M. (2003). The galaxy population in the Coma cluster. s.n. Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 07-10-2021 4 A Catalogue of Galaxies in the Coma Cluster Morphologies, Luminosity Functions and Cluster Dynamics M. Beijersbergen & J. M. van der Hulst ABSTRACT — We present a new multi-color catalogue of 583 spectroscopically confirmed members of the Coma cluster based on a deep wide field survey covering 5.2 deg2. -
The Herschel Sprint PHOTO ILLUSTRATION: PATRICIA GILLIS-COPPOLA, HERSCHEL IMAGE: WIKIMEDIA S&T
The Herschel Sprint PHOTO ILLUSTRATION: PATRICIA GILLIS-COPPOLA, HERSCHEL IMAGE: WIKIMEDIA S&T 34 April 2015 sky & telescope William Herschel’s Extraordinary Night of DiscoveryMark Bratton Recreating the legendary sweep of April 11, 1785 There’s little doubt that William Herschel was the most clearly with his instruments. As we will see, he did make signifi cant astronomer of the 18th century. His accom- occasional errors in interpretation, despite the superior plishments included the discovery of Uranus, infrared optics; for instance, he thought that the planetary nebula radiation, and four planetary satellites, as well as the M57 was a ring of stars. compilation of two extensive catalogues of double and The other factor contributing to Herschel’s interest multiple stars. His most lasting achievement, however, was the success of his sister, Caroline, in her study of the was his exhaustive search for undiscovered star clusters sky. He had built her a small telescope, encouraging her and nebulae, a key component in his quest to understand to search for double stars and comets. She located Messier what he called “the construction of the heavens.” In Her- objects and more, occasionally fi nding star clusters and schel’s time, astronomers were concerned principally with nebulae that had escaped the French astronomer’s eye. the study of solar system objects. The search for clusters Over the course of a year of observing, she discovered and nebulae was, up to that point, a haphazard aff air, with about a dozen star clusters and galaxies, occasionally not- a total of only 138 recorded by all the observers in history. -
Eric Joseph Murphy
Eric Joseph Murphy First-Author 100. Murphy, Eric J. 2013, Astrophysical Journal, 777, 58 Refereed “The Role of Merger Stage on Galaxy Radio Spectra in Local Infrared-Bright Starburst Galaxies” Publications 99. Murphy, E.J., et al. 2013, Astrophysical Journal, 768, 2 “Radio and Mid-Infrared Properties of Compact Starbursts: Distancing Themselves from the Main Sequence” 98. Murphy, E.J., et al. 2012, Astrophysical Journal, 761, 97 “The Star Formation in Radio Survey: GBT 33 GHz Observations of Nearby Galaxy Nuclei and Extranuclear Star-Forming Regions” 97. Murphy, E.J., Porter, T.A., Moskalenko, I.V., Helou, G., and Strong, A.W., 2012, Astrophysical Journal, 750, 126 “Characterizing Cosmic-Ray Propagation in Massive Star-Forming Regions: The Case of 30Doradus and the Large Magellanic Cloud” 96. Murphy, E.J., et al. 2011, Astrophysical Journal, 737, 67 “Calibrating Extinction-Free Star Formation Rate Diagnostics with 33 GHz Free-Free Emission in NGC 6946” 95. Murphy, E.J., Chary, R-.R., Dickinson, M., Pope, A., Frayer, D.T., and Lin, L. 2011, Astrophysical Journal, 732, 126 “An Accounting of the Dust-Obscured Star Formation and Accretion Histories Over the Last ∼11 Billion Years” 94. Murphy, E.J., et al. 2010, Astrophysical Journal Letters, 709, L108 “The Detection of Anomalous Dust Emission in the Nearby Galaxy NGC 6946” 93. Murphy, Eric J. 2009, Astrophysical Journal, 706, 482 “The Far-Infrared–Radio Correlation at High Redshifts: Physical Considerations and Prospects for the Square Kilometer Array” 92. Murphy, E.J., Chary, R.-R., Alexander, D. M., Dickinson, M., Magnelli, B., Morrison, G., Pope, A., and Teplitz, H.