DOCSLIB.ORG

An Atlas of Hubble Space Telescope Ultraviolet Images of Nearby Galaxies

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
An Atlas of Hubble Space Telescope Ultraviolet Images of Nearby Galaxies An Atlas of Hubble Space Telescope Ultraviolet Images of Nearby Galaxies1 Dan Maoz2, Alexei V. Filippenko3, Luis C. Ho3,4, F. Duccio Macchetto5, Hans-Walter Rix6, and Donald P. Schneider7 1 Based on observations with the Hubble Space Telescope which is operated by AURA, Inc., under NASA contract NAS 5-26555 2 School of Physics & Astronomy and Wise Observatory, Tel-Aviv University, Tel-Aviv 69978, Israel. [email protected] 3 Department of Astronomy, University of California, Berkeley, CA 94720-3411 4 Center for Astrophyics, 60 Garden Street, Cambridge, MA 02138 5 Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218 6 Steward Observatory, University of Arizona, Tucson, AZ 85721 7 Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802 ABSTRACT We present an atlas of UV (∼ 2300 A)˚ images, obtained with the Hubble Space Telescope (HST) Faint Object Camera, of the central 22′′ × 22′′ of 110 galaxies. The observed galaxies are an unbiased selection constituting about one half of a complete sample of all large (D > 6′) and nearby (V < 2000 km s−1) galaxies. This is the first extensive UV imaging survey of normal galaxies. The data are useful arXiv:astro-ph/9605170v1 28 May 1996 for studying star formation, low-level nuclear activity, and UV emission by evolved stellar populations in galaxies. At the HST resolution (∼ 0.05′′), the images display an assortment of morphologies and UV brightnesses. These include bright nuclear point sources, compact young star clusters scattered in the field or arranged in circumnuclear rings, centrally-peaked diffuse light distributions, and galaxies with weak or undetected UV emission. We measure the integrated ∼ 2300 A˚ flux in each image, classify the UV morphology, and examine trends between these parameters and the optical properties of the galaxies. Subject headings: atlases – ultraviolet: galaxies – galaxies: structure – galaxies: active – galaxies: star clusters – galaxies: nuclei 1 1. Introduction are probably bound. In a forthcoming work (Ho et al. 1996b) we will use the UV images to analyze the star- Ultraviolet (UV) imaging is a powerful tool for the formation properties of all the galaxies in the sample. study of galaxies. Recent star formation and low- In this paper, we present images and basic data for the level nuclear activity can be traced and measured in 110 galaxies observed. The images provide a reference UV images, unhindered by the bright background of for the UV brightness and morphology of the galaxies the older stellar populations which dominate in visual in the sample, which can be used as a general guide bands. The source of UV emission in some quiescent to the UV properties of the centers of galaxies, and early-type galaxies can also be studied with UV imag- as an aid in extracting the actual data from the HST ing. Prior to the launch of the Hubble Space Telescope archive. We also provide a classification of the UV (HST), few galaxies were imaged in the UV. These few morphology, additional notes on some of the galaxies were mostly Local Group spiral galaxies observed at and what is seen in their images, and a measurement low angular resolution using rocket-borne telescopes of the ∼ 2300 A˚ flux integrated over the image. We on brief flights (see Bohlin et al. 1990, and refer- tabulate these together with the larger-scale proper- ences therein). This situation has improved in recent ties of the galaxies and (for the northern galaxies) years with the flight of UV imaging telescopes on the the spectroscopic nuclear classification from Ho, Fil- Space Shuttle (e.g., Landsman et al. 1992; Hill et ippenko, & Sargent (1995, 1996a). In §2, below, we al. 1992), although the angular resolution is still low describe the sample selection and the observations. In and the number of galaxies observed is small, due to §3 we present tables listing the galaxy parameters, a the limited mission duration. In this respect, HST, pictorial atlas of the data, and notes on some of the with its high sensitivity and angular resolution, has individual galaxies. In §4 we intercompare the UV opened up a new frontier. Summaries of recent HST and optical properties of the galaxies and provide a UV-imaging studies of galaxies appear in Benvenuti, brief summary. Macchetto, & Schreier (1996). We have carried out a UV imaging survey with 2. Observations the pre-COSTAR HST Faint Object Camera (FOC) of the central regions of 110 large nearby galaxies, se- The sample from which the observed galaxies were lected randomly from a complete sample of 240 galax- chosen consists of all galaxies in the UGC and ESO ies. The main purposes of the survey are (a) to de- catalogs (Lauberts & Valentijn 1989) with heliocen- tect low-luminosity active galactic nuclei (AGNs), ex- tric velocities available in the literature and less than ploiting the high contrast of a nuclear UV continuum 2000 km s−1, and photographic diameters (as defined source above the low UV background from stars, and in the catalogs) greater than 6′. A total of 22 galaxies (b) to study star formation in the central regions of were removed from this initial sample of 262 galaxies the galaxies; by observing at ∼ 2300 A,˚ the survey during subsequent stages of the sample definition. In images detect primarily the youngest existing stel- 21 of these, no nuclear position could be defined be- lar populations and thus provide a clean probe of cause they were too diffuse, too low in surface bright- the most recent sites of active star formation, un- ness, or edge-on with strong dust lanes. One galaxy contaminated by light from more evolved stars. The (ESO 1331−4517) had a bright foreground star near power of this technique, especially when augmented the nucleus, which would have endangered the HST by the high HST angular resolution, has been recently instruments. This left a well-defined sample of 240 demonstrated in UV studies of starbursts by Conti & galaxies with observable nuclei. Vacca (1994), Meurer et al. (1995), and Maoz et al. Twenty-seven galaxies from this sample were not (1996). included in our target list because they were proposed Maoz et al. (1995) presented data from the survey targets of other HST UV-imaging programs. How- for nine galaxies displaying bright compact nuclear ever, we have subsequently obtained from the HST UV sources, five of which are potential low-luminosity archive the data for seven of these galaxies which were AGNs. Maoz et al. (1996) analyzed the images of five actually observed with an instrumental configuration additional galaxies having circumnuclear star-forming similar to the one we used (FOC + UV filter at ∼ 2300 rings, and showed that much of the star formation in A).˚ the rings is confined to massive compact clusters that Digitized photographs from the GASP archive at 2 Space Telescope Science Institute (STScI) of all po- have used, the FOC is limited in its dynamic range to tential target galaxies were examined and the coordi- 255 counts (8 bits) per zoomed pixel; additional signal nates of the nucleus determined to ∼ 1′′ −2′′ precision causes the counts to “fold over” and start again from by computing the centroid of the light distribution. In 0. Another problem is that the detected count rate a few cases, as evidenced by the eventual HST images, becomes nonlinear, gradually saturating for bright the galaxy nucleus position was off by up to ∼ 5′′, due sources (see Baxter et al. 1994). The central pix- to isophote distortion by dust features in the GASP els of most of the compact bright sources detected images. in the images may be in the nonlinear regime, and The observations were done in Snapshot mode – the brightest of them are clearly saturated. In sev- i.e., targets were chosen from the target list by the eral galaxies where we report the brightness and/or STScI staff based on the convenience of their location angular size of individual compact sources, our analy- on the sky. The brief exposure was used to fill the sis relies mainly on the wings of the PSF, which have −1 −1 gaps left in the observing schedule after other science low count rates (∼< 0.05 s pixel ), using the algo- programs had been scheduled. The observed galaxies rithms described by Maoz et al. (1995, 1996). We are therefore an unbiased selection from the complete model the PSF using a well-exposed F220W image of sample. a star observed with the FOC f/96 256 × 256 pixel mode, which has a large dynamic and linear range Among the galaxies described in this paper, 103 (but small field of view). Such empirical PSFs are were successfully observed with HST while the pro- required for work in the UV (Baxter et al. 1994). gram was active, in 1993, March through July. We supplement these observations with data for the seven As in Maoz et al. (1995, 1996), we translate the out of the 27 “embargoed” galaxies that were ob- FOC counts to a flux density fλ at 2270 A˚ assuming −1 −17 −1 −2 −1 served with HST between 1991 and 1995. We there- 1 count s =1.66 × 10 erg s cm A˚ , based fore have data for a total of 110 galaxies out of on the on-line calibration data available from STScI the complete sample of 240 galaxies. Observations for the FOC and F220W filter, with a 25% increase in were unsuccessful for four galaxies due to wrong co- sensitivity of the 512 × 1024 zoomed-pixel mode rela- ordinates (NGC 660) or telescope malfunction (NGC tive to the 512 × 512 pixel mode (Baxter et al. 1994).
Load more

Recommended publications
  • The HERACLES View of the H -To-HI Ratio in Galaxies
    The HERACLES View of the H2-to-HI Ratio in Galaxies Adam Leroy (NRAO, Hubble Fellow) Fabian Walter, Frank Bigiel, the HERACLES and THINGS teams The Saturday Morning Summary • Star formation rate vs. gas relation on ~kpc scales breaks apart into: A relatively universal CO-SFR relation in nearby disks Systematic environmental scalings in the CO-to-HI ratio • The CO-to-HI ratio is a strong function of radius, total gas, and stellar surface density correlated with ISM properties: dust-to-gas ratio, pressure harder to link to dynamics: gravitational instability, arms • Interpretation: the CO-to-HI ratio traces the efficiency of GMC formation Density and dust can explain much of the observed behavior heracles Fabian Walter Erik Rosolowsky MPIA UBC Frank Bigiel Eva Schinnerer UC Berkeley THINGS plus… MPIA Elias Brinks Antonio Usero Gaelle Dumas U Hertfordshire OAN, Madrid MPIA Erwin de Blok Andreas Schruba Helmut Wiesemeyer U Cape Town IRAM … MPIA Rob Kennicutt Axel Weiss Karl Schuster Cambridge MPIfR IRAM Barry Madore Carsten Kramer Karin Sandstrom Carnegie IRAM MPIA Michele Thornley Daniela Calzetti Kelly Foyle Bucknell UMass MPIA Collaborators The HERA CO-Line Extragalactic Survey First maps Leroy et al. (2009) • IRAM 30m Large Program to map CO J = 2→1 line • Instrument: HERA receiver array operating at 230 GHz • 47 galaxies: dwarfs to starbursts and massive spirals -2 • Very wide-field (~ r25) and sensitive (σ ~ 1-2 Msun pc ) NGS The HI Nearby Galaxy Survey HI Walter et al. (2008), AJ Special Issue (2008) • VLA HI maps of 34 galaxies:
    [Show full text]
  • Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
    The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al.
    [Show full text]
  • 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.
    [Show full text]
  • 1. Introduction
    THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 122:109È150, 1999 May ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY STRUCTURAL PARAMETERS: STAR FORMATION RATE AND EVOLUTION WITH REDSHIFT M. TAKAMIYA1,2 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637; and Gemini 8 m Telescopes Project, 670 North Aohoku Place, Hilo, HI 96720 Received 1998 August 4; accepted 1998 December 21 ABSTRACT The evolution of the structure of galaxies as a function of redshift is investigated using two param- eters: the metric radius of the galaxy(Rg) and the power at high spatial frequencies in the disk of the galaxy (s). A direct comparison is made between nearby (z D 0) and distant(0.2 [ z [ 1) galaxies by following a Ðxed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broad- band images at D4500A observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between D3000 and D9000A (Williams et al.). The radius is measured from the intensity proÐle of the galaxy using the formulation of Petrosian, and it is argued to be a metric radius that should not depend very strongly on the angular resolution and limiting surface brightness level of the imaging data. It is found that the metric radii of nearby and distant galaxies are comparable to each other.
    [Show full text]
  • CONSTELLATION TRIANGULUM, the TRIANGLE Triangulum Is a Small Constellation in the Northern Sky
    CONSTELLATION TRIANGULUM, THE TRIANGLE Triangulum is a small constellation in the northern sky. Its name is Latin for "triangle", derived from its three brightest stars, which form a long and narrow triangle. Known to the ancient Babylonians and Greeks, Triangulum was one of the 48 constellations listed by the 2nd century astronomer Ptolemy. The celestial cartographers Johann Bayer and John Flamsteed catalogued the constellation's stars, giving six of them Bayer designations. The white stars Beta and Gamma Trianguli, of apparent magnitudes 3.00 and 4.00, respectively, form the base of the triangle and the yellow-white Alpha Trianguli, of magnitude 3.41, the apex. Iota Trianguli is a notable double star system, and there are three star systems with planets located in Triangulum. The constellation contains several galaxies, the brightest and nearest of which is the Triangulum Galaxy or Messier 33—a member of the Local Group. The first quasar ever observed, 3C 48, also lies within Triangulum's boundaries. HISTORY AND MYTHOLOGY In the Babylonian star catalogues, Triangulum, together with Gamma Andromedae, formed the constellation known as MULAPIN "The Plough". It is notable as the first constellation presented on (and giving its name to) a pair of tablets containing canonical star lists that were compiled around 1000 BC, the MUL.APIN. The Plough was the first constellation of the "Way of Enlil"—that is, the northernmost quarter of the Sun's path, which corresponds to the 45 days on either side of summer solstice. Its first appearance in the pre-dawn sky (heliacal rising) in February marked the time to begin spring ploughing in Mesopotamia.
    [Show full text]
  • (HERON) II: the Outer Structure of Edge-On Galaxies
    MNRAS 000,1{19 (2019) Preprint 10 March 2020 Compiled using MNRAS LATEX style file v3.0 The Halos and Environments of Nearby Galaxies (HERON) II: The outer structure of edge-on galaxies Aleksandr Mosenkov,1;2? R. Michael Rich,3 Andreas Koch,4 Noah Brosch,5 David Thilker,6 Javier Rom´an,7 Oliver Muller,¨ 8 Anton Smirnov,9;10 and Pavel Usachev9;11 1Department for Management of Science and Technology Development, Ton Duc Thang University, Ho Chi Minh City, Vietnam 2Faculty of Applied Sciences, Ton Duc Thang University, Ho Chi Minh City, Vietnam 3Department of Physics & Astronomy, Univ. of California Los Angeles, 430 Portola Plaza, Los Angeles, CA 90095-1547, USA 4Zentrum fur¨ Astronomie der Universit¨at Heidelberg, Astronomisches Rechen-Institut, 69120 Heidelberg, Germany 5Wise Observatory, Tel Aviv University, 69978 Tel Aviv, Israel 6Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA 7Instituto de Astrof´ısica de Andaluc´ıa(CSIC), Glorieta de la Astronom´ıa, 18008 Granada, Spain 8Observatoire Astronomique de Strasbourg (ObAS), Universite de Strasbourg - CNRS, UMR 7550 Strasbourg, France 9St. Petersburg State University, Universitetskij pr. 28, 198504 St. Petersburg, Stary Peterhof, Russia 10Central (Pulkovo) Astronomical Observatory, Russian Academy of Sciences, Pulkovskoye Chaussee 65/1, 196140 St. Petersburg, Russia 11Special Astrophysical Observatory, Russian Academy of Sciences, 369167 Nizhnij Arkhyz, Russia Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The HERON project is aimed at studying halos and low surface brightness details near galaxies. In this second HERON paper we consider in detail deep imaging (down to surface brightness of ∼ 28 mag/arcsec2 in the r band) for 35 galaxies, viewed edge- on.
    [Show full text]
  • A Search For" Dwarf" Seyfert Nuclei. VII. a Catalog of Central Stellar
    TO APPEAR IN The Astrophysical Journal Supplement Series. Preprint typeset using LATEX style emulateapj v. 26/01/00 A SEARCH FOR “DWARF” SEYFERT NUCLEI. VII. A CATALOG OF CENTRAL STELLAR VELOCITY DISPERSIONS OF NEARBY GALAXIES LUIS C. HO The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 JENNY E. GREENE1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ ALEXEI V. FILIPPENKO Department of Astronomy, University of California, Berkeley, CA 94720-3411 AND WALLACE L. W. SARGENT Palomar Observatory, California Institute of Technology, MS 105-24, Pasadena, CA 91125 To appear in The Astrophysical Journal Supplement Series. ABSTRACT We present new central stellar velocity dispersion measurements for 428 galaxies in the Palomar spectroscopic survey of bright, northern galaxies. Of these, 142 have no previously published measurements, most being rela- −1 tively late-type systems with low velocity dispersions (∼<100kms ). We provide updates to a number of literature dispersions with large uncertainties. Our measurements are based on a direct pixel-fitting technique that can ac- commodate composite stellar populations by calculating an optimal linear combination of input stellar templates. The original Palomar survey data were taken under conditions that are not ideally suited for deriving stellar veloc- ity dispersions for galaxies with a wide range of Hubble types. We describe an effective strategy to circumvent this complication and demonstrate that we can still obtain reliable velocity dispersions for this sample of well-studied nearby galaxies. Subject headings: galaxies: active — galaxies: kinematics and dynamics — galaxies: nuclei — galaxies: Seyfert — galaxies: starburst — surveys 1. INTRODUCTION tors, apertures, observing strategies, and analysis techniques.
    [Show full text]
  • 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.
    [Show full text]
  • Galaxy Data Name Constell
    Galaxy Data name constell. quadvel km/s z type width ly starsDist. Satellite Milky Way many many 0 0.0000 SBbc 106K 200M 0 M31 Andromeda NQ1 -301 -0.0010 SA 220K 1T 2.54Mly M32 Andromeda NQ1 -200 -0.0007 cE2 Sat. 5K 2.49Mly M31 M110 Andromeda NQ1 -241 -0.0008 dE 15K 2.69M M31 NGC 404 Andromeda NQ1 -48 -0.0002 SA0 no 10M NGC 891 Andromeda NQ1 528 0.0018 SAb no 27.3M NGC 680 Aries NQ1 2928 0.0098 E pec no 123M NGC 772 Aries NQ1 2472 0.0082 SAb no 130M Segue 2 Aries NQ1 -40 -0.0001 dSph/GC?. 100 5E5 114Kly MW NGC 185 Cassiopeia NQ1 -185 -0.0006dSph/E3 no 2.05Mly M31 Dwingeloo 1 Cassiopeia NQ1 110 0.0004 SBcd 25K 10Mly Dwingeloo 2 Cassiopeia NQ1 94 0.0003Iam no 10Mly Maffei 1 Cassiopeia NQ1 66 0.0002 S0pec E3 75K 9.8Mly Maffei 2 Cassiopeia NQ1 -17 -0.0001 SABbc 25K 9.8Mly IC 1613 Cetus NQ1 -234 -0.0008Irr 10K 2.4M M77 Cetus NQ1 1177 0.0039 SABd 95K 40M NGC 247 Cetus NQ1 0 0.0000SABd 50K 11.1M NGC 908 Cetus NQ1 1509 0.0050Sc 105K 60M NGC 936 Cetus NQ1 1430 0.0048S0 90K 75M NGC 1023 Perseus NQ1 637 0.0021 S0 90K 36M NGC 1058 Perseus NQ1 529 0.0018 SAc no 27.4M NGC 1263 Perseus NQ1 5753 0.0192SB0 no 250M NGC 1275 Perseus NQ1 5264 0.0175cD no 222M M74 Pisces NQ1 857 0.0029 SAc 75K 30M NGC 488 Pisces NQ1 2272 0.0076Sb 145K 95M M33 Triangulum NQ1 -179 -0.0006 SA 60K 40B 2.73Mly NGC 672 Triangulum NQ1 429 0.0014 SBcd no 16M NGC 784 Triangulum NQ1 0 0.0000 SBdm no 26.6M NGC 925 Triangulum NQ1 553 0.0018 SBdm no 30.3M IC 342 Camelopardalis NQ2 31 0.0001 SABcd 50K 10.7Mly NGC 1560 Camelopardalis NQ2 -36 -0.0001Sacd 35K 10Mly NGC 1569 Camelopardalis NQ2 -104 -0.0003Ibm 5K 11Mly NGC 2366 Camelopardalis NQ2 80 0.0003Ibm 30K 10M NGC 2403 Camelopardalis NQ2 131 0.0004Ibm no 8M NGC 2655 Camelopardalis NQ2 1400 0.0047 SABa no 63M Page 1 2/28/2020 Galaxy Data name constell.
    [Show full text]
  • The Formation of Spheroids in Early-Type Spirals: Clues from Their Globular Clusters
    To appear in ApJ The Formation of Spheroids in Early-Type Spirals: Clues From Their Globular Clusters1 Aparna Maybhate2, Paul Goudfrooij2, Rupali Chandar3, and Thomas H. Puzia4 ABSTRACT We use deep Hubble Space Telescope images taken with the Advanced Camera for Surveys (ACS) in the F475W and F814W filters to investigate the globular cluster systems in four edge-on Sa spiral galaxies covering a factor of 4 in lumi- nosity. The specific frequencies of the blue globular clusters in the galaxies in our sample fall in the range 0.34 – 0.84, similar to typical values found for later- type spirals. The number of red globular clusters associated with the bulges generally increases with the bulge luminosity, similar to what is observed for el- liptical galaxies, although the specific frequency of bulge clusters is a factor of 2-3 lower for the lowest luminosity bulges than for the higher luminosity bulges. We present a new empirical relation between the fraction of red globular clusters and total bulge luminosity based on the elliptical galaxies studied by ACSVCS (ACS Virgo Cluster Survey), and discuss how this diagram can be used to assess the importance that dissipative processes played in building spiral bulges. Our results suggest a picture where dissipative processes, which are expected during gas-rich major mergers, were more important for building luminous bulges of Sa galaxies, whereas secular evolution may have played a larger role in building lower-luminosity bulges in spirals. Subject headings: galaxies: spiral — galaxies: individual(NGC
    [Show full text]
  • X-Ray Spectral Survey with XMM–Newton of a Complete Sample of Nearby Seyfert Galaxies
    A&A 446, 459–470 (2006) Astronomy DOI: 10.1051/0004-6361:20053893 & c ESO 2006 Astrophysics X-ray spectral survey with XMM–Newton of a complete sample of nearby Seyfert galaxies M. Cappi1, F. Panessa2, L. Bassani1,M.Dadina1, G. DiCocco1, A. Comastri3, R. Della Ceca4, A. V. Filippenko5, F. Gianotti1,L.C.Ho6, G. Malaguti1,J.S.Mulchaey6,G.G.C.Palumbo7, E. Piconcelli8,W.L.W.Sargent9, J. Stephen1, M. Trifoglio1, and K. A. Weaver10 1 INAF-IASF Sezione di Bologna, via Gobetti 101, 40129 Bologna, Italy e-mail: [email protected] 2 Instituto de Fisica de Cantabria (CSIC-UC), Avda de los Castros, 39005 Santander, Spain 3 INAF- Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy 4 INAF- Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy 5 Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA 6 Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA 7 Dipartimento di Astronomia, Universita’ degli Studi di Bologna, via Ranzani 1, 40127 Bologna, Italy 8 XMM–Newton Science Operation Center/RSSD-ESA, Apartado 50727, 28080 Madrid, Spain 9 Department of Astronomy, California Institute of Technology, Pasadena, CA 91125, USA 10 Laboratory for High Energy Astrophysics, NASA’s Goddard Space Flight Center, Greenbelt, MD 20771, USA Received 23 July 2005 / Accepted 28 September 2005 ABSTRACT Results obtained from an X-ray spectral survey of nearby Seyfert galaxies using XMM–Newton are reported. The sample was optically selected, well defined, complete in B magnitude, and distance limited: it consists of the nearest (D ∼< 22 Mpc) 27 Seyfert galaxies (9 of type 1, 18 of type 2) taken from the Ho et al.
    [Show full text]
  • DGSAT: Dwarf Galaxy Survey with Amateur Telescopes
    Astronomy & Astrophysics manuscript no. arxiv30539 c ESO 2017 March 21, 2017 DGSAT: Dwarf Galaxy Survey with Amateur Telescopes II. A catalogue of isolated nearby edge-on disk galaxies and the discovery of new low surface brightness systems C. Henkel1;2, B. Javanmardi3, D. Mart´ınez-Delgado4, P. Kroupa5;6, and K. Teuwen7 1 Max-Planck-Institut f¨urRadioastronomie, Auf dem H¨ugel69, 53121 Bonn, Germany 2 Astronomy Department, Faculty of Science, King Abdulaziz University, P.O. Box 80203, Jeddah 21589, Saudi Arabia 3 Argelander Institut f¨urAstronomie, Universit¨atBonn, Auf dem H¨ugel71, 53121 Bonn, Germany 4 Astronomisches Rechen-Institut, Zentrum f¨urAstronomie, Universit¨atHeidelberg, M¨onchhofstr. 12{14, 69120 Heidelberg, Germany 5 Helmholtz Institut f¨ur Strahlen- und Kernphysik (HISKP), Universit¨at Bonn, Nussallee 14{16, D-53121 Bonn, Germany 6 Charles University, Faculty of Mathematics and Physics, Astronomical Institute, V Holeˇsoviˇck´ach 2, CZ-18000 Praha 8, Czech Republic 7 Remote Observatories Southern Alps, Verclause, France Received date ; accepted date ABSTRACT The connection between the bulge mass or bulge luminosity in disk galaxies and the number, spatial and phase space distribution of associated dwarf galaxies is a dis- criminator between cosmological simulations related to galaxy formation in cold dark matter and generalised gravity models. Here, a nearby sample of isolated Milky Way- class edge-on galaxies is introduced, to facilitate observational campaigns to detect the associated families of dwarf galaxies at low surface brightness. Three galaxy pairs with at least one of the targets being edge-on are also introduced. Approximately 60% of the arXiv:1703.05356v2 [astro-ph.GA] 19 Mar 2017 catalogued isolated galaxies contain bulges of different size, while the remaining objects appear to be bulgeless.
    [Show full text]