DOCSLIB.ORG

Disk Heating

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Disk Heating Constraints on secular evolution in unbarred spiral galaxies: understanding bulge and disk formation April 23rd 2012 July 10th 2012 Marja Kristin Seidel Jesús Falcón - Barroso Instituto de Astrofísica de Canarias www.iac.es/project/traces Constraints on secular evolution in unbarred spiral galaxies: understanding bulge and disk formation disentangling disk heating agents April 23rd 2012 July 10th 2012 Marja Kristin Seidel Jesús Falcón - Barroso Instituto de Astrofísica de Canarias www.iac.es/project/traces [email protected] Introduction: Disk heating More than half of the stellar mass in the local Universe is found in disk galaxies (e.g. Driver et al. 2007) but we are far from understanding them. Especially: What is driving the heating of the disk? Investigate 3D-distribution of stellar velocity dispersions ellipsoid with axes ratios: σz/σR (and σϕ/σR) σz σR Possible disk heating agents: • encounters with giant molecular clouds (GMCs) • scattering by dark halo objects or globular clusters • perturbation by spiral structure • perturbation by stellar bars talk on: www.iac.es/project/traces • dissolution of young stellar clusters • disturbances by satellite galaxies or minor mergers (e.g. from Spitzer & Schwarzschild, 1951 to Saha et al. 2010) [email protected] Introduction: Disk heating Model predictions • encounters with GMCs (Sellwood, 2008): 3D agent • perturbation by spiral structure (Jenkins & Binney, 1990): σR Age • radial migration (e.g. Roskar et al. 2008): σR increases with age Metallicity • for an existing metallicity gradient (e.g. Sánchez-Blázquez, 2009)* : σz/σR increase with metallicity talk on: www.iac.es/project/traces But: in the solar neighborhood little evidence for the age-metallicity-relation (e.g. Feltzing et al., 2001) *still present even with satellites! [email protected] Introduction: Our study Our study focuses on: • 6 disk galaxies across the Hubble sequence • obtaining the ages and metallicities in different regions of the galaxies via full-spectrum fitting techniques • relating these stellar population parameters with earlier kinematic results, i.e. σz/σR and the individual values (Shapiro & Gerssen 2003 and 2012) talk on: www.iac.es/project/traces [email protected] Sample Disk-heating (Shapiro & Gerssen 2003 and 2012) credit: HST/WFPC2 image spectra with resolutions of ~ 30 km s-1 and ~ 23 km s-1 NGC 2280 (Scd) NTT NGC 3810 (Sc) NGC 4030 (Sbc) NGC 1068 (Sb) KPNO NGC 2775 (Sa/Sab) NGC 2460 (Sa) different regions from radial surface brightness profiles and disk scale lengths: center bulge [trans] disk talk on: www.iac.es/project/traces Note: all our galaxies show central sigma drops! [email protected] Methods pPXF (Cappellari & Emsellem, 2004) ; Gandalf (Sarzi et al. 2006) STARLIGHT (Cid Fernandes, 2007) gal_3810mj_cor.fits [Bin 1 ; x = -15.0 ; SN= 15.5] 12 Starlight + Miles models NGC 3810 (Sc) DISKV= 1062.6, != 2.0 km/s (Sánchez-Blazquez et al.2006) gal_3810mj_cor.fits [Bin 1 ; x = -15.0 ; SN= 15.5] 10 12 V= 1062.6, != 2.0 km/s 1.2 8 10 pPXF 6 8 40 1 4 6 2 4 0 500 1000 1500 20 0.8 2 0 500 1000 1500 30 Gandalf 0 0.6 30 +ELODIE 20 (Prugniel et Intensity [arb.units] counts al. 2007) 20 10 0.4 40 counts 10 0 0 500 1000 1500 0 λpixels [Å] 20 0.2 0 500 1000 1500 pixels 0 For all three 4861.33 4958.91 regions 5006.84 in major 5175.36 and 5270.00 minor 5335.00 5406.00 axes: " H [OIII] [OIII] Mgb Fe5270 Fe5335 Fe5406 0 -0.2 10 talk on: www.iac.es/project/traces 4861.33 4958.91 5006.84 5175.36 5270.00 5335.00 ages 5406.00 " mass &H luminosity[OIII] [OIII] weightedMgb Fe5270 Fe5335 Fe5406 4800 5000 5200 5400 0 5 10 15 8 metallicities 10 6 8 Counts Analyze4 the stellar populations! 6 2 Counts 4 0 4800 5000 5200 5400 2 Restwavelength [Angstroms] 0 4800 5000 5200 5400 Restwavelength [Angstroms] How can stellar populations help us to understand • secular evolution in spirals? • disk heating processes? [email protected] Preliminary results: Ages and [Fe/H] Luminosity weighted Mass weighted age [Gyr] [Fe / H] repr. error 250 center bulge disk center bulge disk Sa Sab Young populations dominate the luminosity weighted age (e.g. Serra & Trager, 2006) talk on: www.iac.es/project/traces Sb Sbc We mostly confirm inside-out growth scenario (e.g. Muños-Mateos, 2007) 200 Sc In our sample: late types show stronger [Fe/H] gradients than the early types Scd (adding to MacArthur et al., 2009) R ! 150 100 50 0 5 10 15 20 age [Gyr] [email protected] Preliminary results: Ages and [Fe/H] Luminosity weighted Mass weighted age [Gyr] [Fe / H] repr. error 250 center bulge disk center bulge disk Sa Sab Young populations dominate the luminosity weighted age (e.g. Serra & Trager, 2006) talk on: www.iac.es/project/traces Sb Sbc We mostly confirm inside-out growth scenario (e.g. Muños-Mateos, 2007) 200 Sc In our sample: late types show stronger [Fe/H] gradients than the early types Scd (adding to MacArthur et al., 2009) R ! 150 100 50 0 5 10 15 20 age [Gyr] [email protected] Preliminary results: Disk heating With our stellar population results: 6 J.Gerssen & K. Shapiro Griffin is it possible to relate these two findings?Evolutionary stellar population synthesis 1659 Z B-V talk on: www.iac.es/project/traces Figure 4. Velocity ellipsoid ratio σz/σR as a function of galactic Figure 5. Velocity ellipsoid ratio σz/σR as a function of type (Hubble stage T). The solid points show the results that inclination- and extinction-corrected galaxy colour (available in age [Gyr] Figure 19. We plot the broad-band B V colour derived from the SSP we obtained previously (Shapiro et al. 2003). The results that we HyperLeda for 7 of our 8 spirals and the fast-rotating E/S0s). The − derive in this paper for two late type spirals are shown as the black points indicate our spiral galaxy data, and the red squaresSEDs for different ages and metallicities (as indicated within the panel) and Gerssen & Shapiro, 2012 the KroupaVazdekis universal IMF with et the al., zero-point 2010 set with two different Vega Figure 17. Variation of Balmer line-strength indices with metallicity pre- open circles. Horizontal errors represent the uncertainty inherent are the data of Cappellari et al. (2007) for fast-rotating E andspectra in black (very thin) and red (thicker) (see the text for details). The dicted by our single stellar population models of 10 Gyr and Kroupa uni- thickest green line represents the photometric colour computed by Vazdekis in galaxy classification (Naim et al. 1995). The filled square is the S0 galaxies.versal The IMF. linear Different fit line (dashed styles show line) predictions is to for theindices spiral measured gala at xies et al. (1996), as updated in this work, which is based on extensive empirical value in the Solar Neighbourhood derived from Hipparcos data only. The probabilitydifferent spectral of resolutions, no correlation, as in Fig. 14. null hypothesis H , is one 0 photometric stellar libraries. (Dehnen & Binney 1998). percent. of 4300 Å are significantly larger than for the redder part of the units (IFUs) to observe velocity dispersions in disk galaxies. “fast rotators,” are bulge-dominated galaxies that neverthe-spectra∼ for all the clusters. We do not discard possible effects due to This is observationally more efficient than obtaining long-slit less contain a significant disk component (Kuntschner et al.the fact that the Milky Way GCs show oxygen-enhanced abundance spectra, one at a time, along two (or more) position angles. ratios for low metallicities. In fact, Cassisi et al. (2004) have shown 2006; Krajnovi´cet al. 2008). It is therefore interesting tothat such effects become relevant for the spectral ranges covered by Additionally, since IFUs uniformly sample velocity disper- investigate how the disks of these early-type galaxies arethe B, and mostly U, broad-band filters. Therefore, an appropriate sions along both azimuth and radius across the disk, the related to those in spiral galaxies. modelling for these clusters requires working with such α-enhanced assumption of the epicycle approximation, employed here stellar evolutionary isochrones as well as the use of stellar spectra Cappellari et al. (2007) have used axisymmetricwith a similar abundance pattern. In addition, we also require to for long-slit data, can be relaxed. Noordermeer et al. (2008) Schwarzschild dynamical models to extract the three-use specific stellar spectra with CN-strong absorption features and use the PPAK IFU to explore velocity dispersions in disk dimensional orbital structure of a subsample of theCN-enhanced isochrones. galaxies and to constrain the shape of the velocity ellipsoid In Fig. 21, we show our SED fit to the integrated spectrum of SAURON galaxies and measure the shape of their velocitythe standard open cluster M67 (Schiavon, Caldwell & Rose 2004). in one system, NGC 2985. Their measurement of σz/σR ellipsoids. These anisotropy measurements are luminosity-Unlike for the GCs of Fig. 20, these authors obtained the integrated ≈ 0.7 is consistent with our previous result for this sys- weighted, giving more weight to the high-density equatorialspectrum for M67 by co-adding individual spectra of cluster mem- tem (0.75 ± 0.09; Gerssen et al. 2000) and confirms that the bers, weighted according to their luminosities and relative numbers. plane, and volume-averaged, giving more weight to largerThe age and metallicity obtained are in good agreement with these epicycle theory we assume is indeed applicable in this galaxy. radii; as aFigure result, 18. Comparison the global of the Hβ anisotropiesindex computed on (see the basis table of the 2 ofauthors (see also Schiavon 2007) and with our isochrone fitting re- In a series of conference proceedings Westfall et al.
Load more

Recommended publications
  • 190 Index of Names
    Index of names Ancora Leonis 389 NGC 3664, Arp 005 Andriscus Centauri 879 IC 3290 Anemodes Ceti 85 NGC 0864 Name CMG Identification Angelica Canum Venaticorum 659 NGC 5377 Accola Leonis 367 NGC 3489 Angulatus Ursae Majoris 247 NGC 2654 Acer Leonis 411 NGC 3832 Angulosus Virginis 450 NGC 4123, Mrk 1466 Acritobrachius Camelopardalis 833 IC 0356, Arp 213 Angusticlavia Ceti 102 NGC 1032 Actenista Apodis 891 IC 4633 Anomalus Piscis 804 NGC 7603, Arp 092, Mrk 0530 Actuosus Arietis 95 NGC 0972 Ansatus Antliae 303 NGC 3084 Aculeatus Canum Venaticorum 460 NGC 4183 Antarctica Mensae 865 IC 2051 Aculeus Piscium 9 NGC 0100 Antenna Australis Corvi 437 NGC 4039, Caldwell 61, Antennae, Arp 244 Acutifolium Canum Venaticorum 650 NGC 5297 Antenna Borealis Corvi 436 NGC 4038, Caldwell 60, Antennae, Arp 244 Adelus Ursae Majoris 668 NGC 5473 Anthemodes Cassiopeiae 34 NGC 0278 Adversus Comae Berenices 484 NGC 4298 Anticampe Centauri 550 NGC 4622 Aeluropus Lyncis 231 NGC 2445, Arp 143 Antirrhopus Virginis 532 NGC 4550 Aeola Canum Venaticorum 469 NGC 4220 Anulifera Carinae 226 NGC 2381 Aequanimus Draconis 705 NGC 5905 Anulus Grahamianus Volantis 955 ESO 034-IG011, AM0644-741, Graham's Ring Aequilibrata Eridani 122 NGC 1172 Aphenges Virginis 654 NGC 5334, IC 4338 Affinis Canum Venaticorum 449 NGC 4111 Apostrophus Fornac 159 NGC 1406 Agiton Aquarii 812 NGC 7721 Aquilops Gruis 911 IC 5267 Aglaea Comae Berenices 489 NGC 4314 Araneosus Camelopardalis 223 NGC 2336 Agrius Virginis 975 MCG -01-30-033, Arp 248, Wild's Triplet Aratrum Leonis 323 NGC 3239, Arp 263 Ahenea
    [Show full text]
  • Making a Sky Atlas
    Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it.
    [Show full text]
  • Ngc Catalogue Ngc Catalogue
    NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39
    [Show full text]
  • On the Morphology of Sigma-Drop Galaxies
    A&A 485, 695–705 (2008) Astronomy DOI: 10.1051/0004-6361:20079161 & c ESO 2008 Astrophysics On the morphology of sigma-drop galaxies S. Comerón1,J.H.Knapen1, and J. E. Beckman1,2 1 Instituto de Astrofísica de Canarias, 38200 La Laguna, Spain e-mail: [email protected] 2 Consejo Superior de Investigaciones Científicas, Spain Received 28 November 2007 / Accepted 28 April 2008 ABSTRACT Context. Local reductions of the stellar velocity dispersion in the central regions of galaxies are known as sigma-drops (σ-drops). Knowing the origin of these features can lead to better understanding of inner galactic dynamics. Aims. We present a sample of 20 σ-drop galaxies matched with a control sample of galaxies without σ-drop in order to search for correlations between σ-drops and the properties, primarily morphological, of the nuclear zones and discs of their host galaxies. Methods. We study the dust and Hα distribution at 0.1 arcsec scale, using Hubble Space Telescope imaging, in the circumnuclear zones of the two samples of galaxies, searching for differences and trying to establish a link between the nuclear kinematics and the host morphology. We have also considered the CO and H i emission of the galaxies and their luminosity profiles. Results. We classify the two samples following both morphological parameters and the luminosity profiles. We find a larger fraction of nuclear dust spirals and Hα rings in the σ-drop sample. We also find that the fraction of Seyfert galaxies in the σ-drop sample is bigger than that of LINERs and that the reverse is true for the control sample.
    [Show full text]
  • Atlante Grafico Delle Galassie
    ASTRONOMIA Il mondo delle galassie, da Kant a skylive.it. LA RIVISTA DELL’UNIONE ASTROFILI ITALIANI Questo è un numero speciale. Viene qui presentato, in edizione ampliata, quan- [email protected] to fu pubblicato per opera degli Autori nove anni fa, ma in modo frammentario n. 1 gennaio - febbraio 2007 e comunque oggigiorno di assai difficile reperimento. Praticamente tutte le galassie fino alla 13ª magnitudine trovano posto in questo atlante di più di Proprietà ed editore Unione Astrofili Italiani 1400 oggetti. La lettura dell’Atlante delle Galassie deve essere fatto nella sua Direttore responsabile prospettiva storica. Nella lunga introduzione del Prof. Vincenzo Croce il testo Franco Foresta Martin Comitato di redazione e le fotografie rimandano a 200 anni di studio e di osservazione del mondo Consiglio Direttivo UAI delle galassie. In queste pagine si ripercorre il lungo e paziente cammino ini- Coordinatore Editoriale ziato con i modelli di Herschel fino ad arrivare a quelli di Shapley della Via Giorgio Bianciardi Lattea, con l’apertura al mondo multiforme delle altre galassie, iconografate Impaginazione e stampa dai disegni di Lassell fino ad arrivare alle fotografie ottenute dai colossi della Impaginazione Grafica SMAA srl - Stampa Tipolitografia Editoria DBS s.n.c., 32030 metà del ‘900, Mount Wilson e Palomar. Vecchie fotografie in bianco e nero Rasai di Seren del Grappa (BL) che permettono al lettore di ripercorrere l’alba della conoscenza di questo Servizio arretrati primo abbozzo di un Universo sempre più sconfinato e composito. Al mondo Una copia Euro 5.00 professionale si associò quanto prima il mondo amatoriale. Chi non è troppo Almanacco Euro 8.00 giovane ricorderà le immagini ottenute dal cielo sopra Bologna da Sassi, Vac- Versare l’importo come spiegato qui sotto specificando la causale.
    [Show full text]
  • Spiral Galaxies with HST/NICMOS. I. Nuclear Morphologies, Color Maps and Distinct Nuclei1
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Spiral Galaxies with HST/NICMOS. I. Nuclear Morphologies, Color Maps and Distinct Nuclei1 C. Marcella Carollo2 Columbia University, Department of Astronomy, 538 W. 120th St., New York, NY 10027 Massimo Stiavelli Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218 Marc Seigar3 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281, B-9000 Gent, Belgium Space Telescope Science Institute, 3700 San Martin Drive, Baltimore MD 21218 P. Tim de Zeeuw Sterrewacht Leiden, Postbus 9513, 2300 RA Leiden, The Netherlands Herwig Dejonghe Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281, B-9000 Gent, Belgium Received ; accepted 1Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by Association of Universities for Research in Astronomy, Inc. (AURA), under NASA contract NAS5-26555 2Visiting Astronomer, The Johns Hopkins University, Department of Physics and Astronomy, Baltimore MD 21210 3Joint Astronomy Centre, 660 N. A’ohoku Place, Hilo, HI 96720 –2– ABSTRACT This is the first of two papers where we present the analysis of an HST NICMOS-Cam2 near-infared (NIR) snapshot survey in the F160W (H) filter for a sample of 78 spiral galaxies selected from the UGC and ESOLV catalogs. For 69 of these objects we provide nuclear color information derived by combining the H data either with additional NICMOS F110W (J) images or with V WFPC2/HST data. Here we present the NIR images and the optical-NIR color maps. We focus our attention on the properties of the photometrically-distinct ‘nuclei’ which are found embedded in most of the galaxies, and provide measurements of their half-light radii and magnitudes in the H (and when available, in the J) band.
    [Show full text]
  • Circumnuclear Dust in Nearby Active and Inactive Galaxies. I. Data1
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server ApJS Accepted [21 Oct 2002] Circumnuclear Dust in Nearby Active and Inactive Galaxies. I. Data1 Paul Martini 2, Michael W. Regan 3 John S. Mulchaey 2, Richard W. Pogge4, ABSTRACT 1Based on observations with the NASA/ESA Hubble Space Telescope obtained at the the Space Tele- scope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. 2Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101-1292, [email protected], [email protected] 3Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, [email protected] 4Department of Astronomy, Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, [email protected] –2– The detailed morphology of the interstellar medium (ISM) in the central kilo- parsec of galaxies is controlled by pressure and gravitation. The combination of these forces shapes both circumnuclear star formation and the growth of the cen- tral, supermassive black hole. We present visible and near-infrared Hubble Space Telescope images and color maps of 123 nearby galaxies that show the distribu- tion of the cold ISM, as traced by dust, with excellent spatial resolution. These observations reveal that nuclear dust spirals are found in the majority of active and inactive galaxies and they possess a wide range in coherence, symmetry, and pitch angle. We have used this large sample to develop a classification system for circumnuclear dust structures. In spite of the heterogeneous nature of the com- plete sample, we only find symmetric, two-arm nuclear dust spirals in galaxies with large scale bars and these dust lanes clearly connect to dust lanes along the leading edges of the large scale bars.
    [Show full text]
  • A Classical Morphological Analysis of Galaxies in the Spitzer Survey Of
    Accepted for publication in the Astrophysical Journal Supplement Series A Preprint typeset using LTEX style emulateapj v. 03/07/07 A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) Ronald J. Buta1, Kartik Sheth2, E. Athanassoula3, A. Bosma3, Johan H. Knapen4,5, Eija Laurikainen6,7, Heikki Salo6, Debra Elmegreen8, Luis C. Ho9,10,11, Dennis Zaritsky12, Helene Courtois13,14, Joannah L. Hinz12, Juan-Carlos Munoz-Mateos˜ 2,15, Taehyun Kim2,15,16, Michael W. Regan17, Dimitri A. Gadotti15, Armando Gil de Paz18, Jarkko Laine6, Kar´ın Menendez-Delmestre´ 19, Sebastien´ Comeron´ 6,7, Santiago Erroz Ferrer4,5, Mark Seibert20, Trisha Mizusawa2,21, Benne Holwerda22, Barry F. Madore20 Accepted for publication in the Astrophysical Journal Supplement Series ABSTRACT The Spitzer Survey of Stellar Structure in Galaxies (S4G) is the largest available database of deep, homogeneous middle-infrared (mid-IR) images of galaxies of all types. The survey, which includes 2352 nearby galaxies, reveals galaxy morphology only minimally affected by interstellar extinction. This paper presents an atlas and classifications of S4G galaxies in the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. The CVRHS system follows the precepts of classical de Vaucouleurs (1959) morphology, modified to include recognition of other features such as inner, outer, and nuclear lenses, nuclear rings, bars, and disks, spheroidal galaxies, X patterns and box/peanut structures, OLR subclass outer rings and pseudorings, bar ansae and barlenses, parallel sequence late-types, thick disks, and embedded disks in 3D early-type systems. We show that our CVRHS classifications are internally consistent, and that nearly half of the S4G sample consists of extreme late-type systems (mostly bulgeless, pure disk galaxies) in the range Scd-Im.
    [Show full text]
  • Camelopardalis Giraffe
    Lateinischer Name: Deutscher Name: Cam Camelopardalis Giraffe Atlas Karte (2000.0) Kulmination um Cambridge Star 1, 3 Mitternacht: Atlas 1, 2, 3, 4, Cam_chart.gif Sky Atlas 5 Cam_chart.gif 23. Dezember Deklinationsbereich: 53° ... 86° Fläche am Himmel: 757° 2 Benachbarte Sternbilder: Aur Cas Cep Dra Lyn Per UMa UMi Geschichte: Die Giraffe wurde erst zu Beginn des 17. Jahrhunderts in die Sternbilderkunde eingeführt und hat somit keinen mythologischen Hintergrund. Das Sternbild wird meist dem holländischen Astronomen Petrus Plancius zugeschrieben, doch hat der Mathematiker Jakob Bartsch , ein Schwiegersohn Johannes Kepler , es bereits 1624 in einem Buch erwähnt. Dieser jeder dichterischen Phantasie bare Mathematiker taufte in seinem Werk Usus astronomicus planisphaerium Argentinae diese amorphe Stelle am Himmel auf den Namen "Giraffe". Die Giraffe war im antiken Griechenland unter dem Begriff "Leoparden-Kamel" bekannt. Jakob Bartsch zog es vor, das Sternbild als Kamel zu bezeichnen, namentlich das Kamel, welches Rebekka von Haran nach Kanaan brachte um Isaak zu heiraten. (Genesis 24:61). Weitere von Bartsch benannte Sternbilder sind Columba und Monoceros . Da die Astronomen ungern einmal eingebürgerte Sternbildnamen ändern, blieb Camelopardalis (auch Camelopardus) bis auf den heutigen Tag erhalten. [bk7 , bk21 , dq1 ] Sternbild: Zwischen dem Sternbild Auriga und dem Polarstern klafft am Firmament eine Stelle gähnender Leere. Nur wenige Sterne erreichen eine Helligkeit, die unser Auge fesseln und zu einer Assoziation verleiten würde. Gerade
    [Show full text]
  • The Full Appendices with All References
    Breakthrough Listen Exotica Catalog References 1 APPENDIX A. THE PROTOTYPE SAMPLE A.1. Minor bodies We classify Solar System minor bodies according to both orbital family and composition, with a small number of additional subtypes. Minor bodies of specific compositions might be selected by ETIs for mining (c.f., Papagiannis 1978). From a SETI perspective, orbital families might be targeted by ETI probes to provide a unique vantage point over bodies like the Earth, or because they are dynamically stable for long periods of time and could accumulate a large number of artifacts (e.g., Benford 2019). There is a large overlap in some cases between spectral and orbital groups (as in DeMeo & Carry 2014), as with the E-belt and E-type asteroids, for which we use the same Prototype. For asteroids, our spectral-type system is largely taken from Tholen(1984) (see also Tedesco et al. 1989). We selected those types considered the most significant by Tholen(1984), adding those unique to one or a few members. Some intermediate classes that blend into larger \complexes" in the more recent Bus & Binzel(2002) taxonomy were omitted. In choosing the Prototypes, we were guided by the classifications of Tholen(1984), Tedesco et al.(1989), and Bus & Binzel(2002). The comet orbital classifications were informed by Levison(1996). \Distant minor bodies", adapting the \distant objects" term used by the Minor Planet Center,1 refer to outer Solar System bodies beyond the Jupiter Trojans that are not comets. The spectral type system is that of Barucci et al. (2005) and Fulchignoni et al.(2008), with the latter guiding our Prototype selection.
    [Show full text]
  • Kinematic Signatures of Bulges Correlate with Bulge Morphologies and Sersic´ Index∗
    The Astrophysical Journal, 754:67 (27pp), 2012 July 20 doi:10.1088/0004-637X/754/1/67 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. KINEMATIC SIGNATURES OF BULGES CORRELATE WITH BULGE MORPHOLOGIES AND SERSIC´ INDEX∗ Maximilian H. Fabricius1,2, Roberto P. Saglia1,DavidB.Fisher3, Niv Drory4, Ralf Bender1,2, and Ulrich Hopp1,2 1 Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, D-85748 Garching, Germany 2 University Observatory Munich, Schienerstrasse 1, D-81679 Munich, Germany 3 Laboratory of Millimeter Astronomy, University of Maryland, College Park, MD 29742, USA 4 Instituto de Astronomia, Universidad Nacional Autonoma de Mexico (UNAM), A.P. 70-264, 04510 Mexico, D.F., Mexico Received 2011 August 30; accepted 2012 April 20; published 2012 July 6 ABSTRACT We use the Marcario Low Resolution Spectrograph at the Hobby–Eberly Telescope to study the kinematics of pseudobulges and classical bulges in the nearby universe. We present major axis rotational velocities, velocity −1 dispersions, and h3 and h4 moments derived from high-resolution (σinst ≈ 39 km s ) spectra for 45 S0 to Sc galaxies; for 27 of the galaxies we also present minor axis data. We combine our kinematics with bulge-to-disk decompositions. We demonstrate for the first time that purely kinematic diagnostics of the bulge dichotomy agree systematically with those based on Sersic´ index. Low Sersic´ index bulges have both increased rotational support (higher v/σ values) and on average lower central velocity dispersions. Furthermore, we confirm that the same correlation also holds when visual morphologies are used to diagnose bulge type.
    [Show full text]
  • Seen Galaxies Count Ref1 Ref2 Con Visual Scale Mag SBR SIZE M Distance Rv Dist COMMENTS
    Seen galaxies Count ref1 ref2 con visual_scale mag SBR SIZE_M Distance Rv dist COMMENTS 1. NGC 224 M 31 AND 5 3.4 13.5 189 2.6 -14 Very large and bright 2. NGC 3031 M 81 UMA 4 6.9 13.2 24.9 12 -3 Fine large galaxy 3. NGC 598 M 33 TRI 3 5.7 14.2 68.7 2.8 -10 Large faint glow in square of stars 4. NGC 4594 M 104 VIR 3 8.0 11.6 8.6 30 48 Moon therefore little detail 5. NGC 221 M 32 AND 3 8.1 12.4 8.5 2.6 -10 Small but easy to see 6. NGC 4472 M 49 VIR 3 8.4 13.2 9.8 53 43 Lovely fuzzy galaxy 7. NGC 3034 M 82 UMA 3 8.4 12.5 10.5 12 13 Could make out bright and dark patches 8. NGC 4258 M 106 CVN 3 8.4 13.6 17.4 24 21 Fine large oval galaxy. So much brighter than most I have been looking at recently. 9. NGC 4826 M 64 COM 3 8.5 12.7 10.3 24 21 Easy galaxy to see 10. NGC 4486 M 87 VIR 3 8.6 13 8.7 51 57 Bright ball 11. NGC 4649 M 60 VIR 3 8.8 12.9 7.6 54 49 Lovely view with three galaxies visible. M60 is the brightest of the three. A nice bright ball of stars 12. NGC 3115 MCG - 1-26- 18 SEX 3 8.9 11.9 7.3 33 29 Bright spindle 13.
    [Show full text]