DOCSLIB.ORG

On the Relation Between Circular Velocity and Central Velocity Dispersion in High and Low Surface Brightness Galaxies1 A

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
On the Relation Between Circular Velocity and Central Velocity Dispersion in High and Low Surface Brightness Galaxies1 A The Astrophysical Journal, 631:785–791, 2005 October 1 A # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. ON THE RELATION BETWEEN CIRCULAR VELOCITY AND CENTRAL VELOCITY DISPERSION IN HIGH AND LOW SURFACE BRIGHTNESS GALAXIES1 A. Pizzella,2 E. M. Corsini,2 E. Dalla Bonta`,2 M. Sarzi,3 L. Coccato,2 and F. Bertola2 Received 2005 January 5; accepted 2005 March 24 ABSTRACT In order to investigate the correlation between the circular velocity Vc and the central velocity dispersion of the spheroidal component c , we analyzed these quantities for a sample of 40 high surface brightness (HSB) disk galaxies, eight giant low surface brightness (LSB) spiral galaxies, and 24 elliptical galaxies characterized by flat À1 À1 rotation curves. Galaxies have been selected to have a velocity gradient 2kms kpc for R 0:35R25.Weused these data to better define the previous Vc-c correlation for spiral galaxies (which turned out to be HSB) and elliptical galaxies, especially at the lower end of the c values. We find that the Vc-c relation is described by a linear À1 law out to velocity dispersions as low as c 50 km s , while in previous works a power law was adopted for À1 galaxies with c > 80 km s . Elliptical galaxies with Vc based on dynamical models or directly derived from the H i rotation curves follow the same relation as the HSB galaxies in the Vc-c plane. On the other hand, the LSB galaxies follow a different relation, since most of them show either higher Vc or lower c with respect to the HSB galaxies. This argues against the relevance of baryon collapse to the radial density profile of the dark matter halos of LSB galaxies. Moreover, if the Vc-c relation is equivalent to one between the mass of the dark matter halo and that of the supermassive black hole, then these results suggest that the LSB galaxies host a supermassive black hole (SMBH) with a smaller mass compared to HSB galaxies with an equal dark matter halo. On the other hand, if the fundamental correlation of SMBH mass is with the halo circular velocity, then LSB galaxies should have larger black hole masses for a given bulge dispersion. Elliptical galaxies with Vc derived from H i data and LSB galaxies were not considered in previous studies. Subject headings: black hole physics — galaxies: elliptical and lenticular, cD — galaxies: fundamental parameters — galaxies: halos — galaxies: kinematics and dynamics — galaxies: spiral Online material: color figure 1. INTRODUCTION fective radius. As a consequence, the maximum circular veloc- A possible relation between the central velocity dispersion ity is correlated with the central velocity dispersion of the gal- axy (Gerhard et al. 2001). Whether the same is true for more of the spheroidal component ( ) and the galaxy circular veloc- c flattened and fainter elliptical galaxies is still to be investigated. ity measured in the flat region of the rotation curve (V )was c On the other hand, both the shape and amplitude of the rota- suggested by Whitmore et al. (1979) and Whitmore & Kirshner tion curve of a spiral galaxy depend on the galaxy luminosity (1981). By measuring H i line widths, they found that V / 1:7 c c and morphological type (e.g., Burstein & Rubin 1985; Persic for a sample of S0 and spiral galaxies. Recently, Ferrarese (2002) et al.1996). For this reason, for spiral galaxies the V - relation proceeded further, extending the V - relation to elliptical gal- c c c c is not expected a priori. axies. She interpreted the V - relation as suggestive of a c c It is interesting to investigate whether the V - relation also correlation between two different galactic components, since c c holds for less dense objects characterized by a less steep po- c and Vc probe the potential of the spheroidal component and of the dark matter (DM) halo, respectively. In particular, it re- tential well. This is the case for low surface brightness (LSB) galaxies, which are disk galaxies with a central face-on surface sults that for a given DM halo the central velocity dispersion of brightness 22:6 mag arcsecÀ2 (e.g., Schombert et al. 1992; the spheroidal component is independent of the morphological B Impey et al. 1996). Previous work concentrated on high surface type. The validity of this relation has been confirmed by Baes brightness (HSB) galaxies, and to infer the V for elliptical gal- et al. (2003), who enlarged the sample of spiral galaxies. c axies, they relied on stellar dynamical models. In this work we For elliptical galaxies, V is generally inferred by means c investigate the behavior of elliptical galaxies with H i–based V of dynamical modeling of the stellar kinematics. This is the c and of LSB galaxies in the V - relation. case for the giant round and almost nonrotating elliptical gal- c c This paper is organized as follows. An overview of the axies studied by Kronawitter et al. (2000). These galaxies form properties of the sample galaxies, as well as an analysis of the a unique dynamical family that scales with luminosity and ef- kinematic data available in the literature to derive their Vc and c, are presented in x 2. The results and discussion concerning 1 Based on observations made with European Southern Observatory tele- the Vc-c relation are given in x 3. scopes at the Paranal Observatory under programs 67.B-0283, 69.B-0573, and 70.B-0171. 2. SAMPLE SELECTION 2 Dipartimento di Astronomia, Universita` di Padova, vicolo dell’Osserva- torio 2, I-35122 Padova, Italy. In the past years we started a scientific program aimed at 3 Physics Department, University of Oxford, Keble Road, Oxford OX1 deriving the detailed kinematics of ionized gas and stars in HSB 3RH, UK. and LSB galaxies in order to study their mass distributions and 785 786 PIZZELLA ET AL. Fig. 1.—Deprojected rotation curves of the eight LSB galaxies of the final sample. structural properties. We measured the velocity curves and that were not characterized by an outer flat portion. Ferrarese velocity dispersion profiles along the major axis for both the (2002) and Baes et al. (2003) considered galaxies with the ro- ionized-gas and stellar components for a preliminary sample tation curve extending farther out than R25. This criterion is not of 50 HSB galaxies (10 S0–S0/a galaxies in Corsini et al. appropriate when the sample of galaxies spans a wide range in [2003]; seven Sa galaxies in Bertola et al. [1996] and Corsini photometric properties. For LSB galaxies, which have a lower et al. [1999]; 16 S0–Sc galaxies in Vega Beltra´n et al. [2001]; central surface brightness than HSB galaxies, R25 corresponds and 17 Sb–Scd galaxies in Pizzella et al. [2004b]) and 11 LSB to a relatively small radius, where the rotation curve may be still galaxies (A. Pizzella et al. 2005, in preparation; Pizzella et al. rising. For this reason we adopt a criterion that selects rota- 2004a). tion curves on the basis of their flatness rather then on their The HSB sample consists of disk galaxies with Hubble type extension. ranging from S0 to Scd, an inclination i 30, and a distance The flatness of each rotation curve has been checked by D < 80 Mpc. The LSB sample consists of disk galaxies with fitting it with a linear law, V(R) ¼ AR þ B for R 0:35R25. Hubble type ranging from Sa to Irr, an intermediate inclina- The radial range has been chosen in order to avoid the bulge- tion (30 P i < 70), and a distance D < 65 Mpc (except for ESO dominated region of the rotation curve (e.g., IC 724 and NGC 534-G20). Three LSB galaxies, namely, ESO 206-G14, ESO 2815). The rotation curves with jAj2kmsÀ1 kpcÀ1 within 488-G49, and LSBC F563-V02, have been selected from the 3 have been considered not to be flat. In this way 15 HSB gal- sample observed by de Blok & McGaugh (1997). The remain- axies and eight LSB galaxies resulted as having a flat rotation ing eight objects are LSB galaxies with bulge. They have been curve. Since the velocity curves of the LSB galaxies were not pre- selected in Lauberts & Valentijn (1989, hereafter ESO-LV) to sented in previous papers, we show their folded rotation curves have a LSB disk component following the criteria described by in Figure 1. We derived Vc by averaging the outermost values of Beijersbergen et al. (1999). Due to the bulge light contribution, the flat portion of the rotation curve. the total central face-on surface brightness of the galaxy could be We are therefore confident that we are giving a reliable es- À2 B 22:6 mag arcsec . However, all these objects do have a timate of the asymptotic value of the circular velocity that traces LSB disk. As far as their total luminosity is concerned, LSBC the mass of the DM halo (for a discussion, see Ferrarese 2002). F563-V02 and ESO 488-G49 are two dwarf LSB galaxies, but We derived c from the stellar kinematics by extrapolating the the other nine objects are representative of giant LSB galaxies velocity dispersion radial profile to r ¼ 000. This has been done (e.g., McGaugh et al. 2001). by fitting the eight innermost data points with an empirical func- For all the HSB and LSB galaxies, we obtained the ionized- tion (either an exponential, a Gaussian, or a constant). We did not gas rotation curve by folding the observed line-of-sight ve- apply any aperture correction to c, as discussed by Baes et al.
Load more

Recommended publications
  • A Multivariate Statistical Analysis of Spiral Galaxy Luminosities. I. Data and Results
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server A Multivariate Statistical Analysis of Spiral Galaxy Luminosities. I. Data and Results Alice Shapley California Institute of Technology, Pasadena CA, 91125, USA G. Fabbiano Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 P. B. Eskridge Ohio State University, Dept. of Astronomy, 140 W 18th Ave, Columbus, OH 43210 ABSTRACT We have performed a multiparametric analysis of luminosity data for a sample of 234 normal spiral and irregular galaxies observed in X-rays with the Einstein Observatory. This sample is representative of S and Irr galaxies, with a good coverage of morphological types and absolute magnitudes. In addition to X-ray and optical data, we have compiled H-band magnitudes, IRAS near- and far-infrared, and 6cm radio continuum observations for the sample from the literature. We have also performed a careful compilation of distance estimates. We have explored the effect of morphology by dividing the sample into early (S0/a-Sab), intermediate (Sb-Sbc), and late-type (Sc-Irr) subsamples. The data were analysed with bivariate and multivariate survival analysis techniques that make full use of all the information available in both detections and limits. We find that most pairs of luminosities are correlated when considered individually, and this is not due to a distance bias. Different luminosity-luminosity correlations follow different power-law relations. Contrary to previous reports, the LX LB correlation follows a power-law with exponent − larger than 1. Both the significances of some correlations and their power-law relations are morphology dependent.
    [Show full text]
  • Observational Studies of the Galaxy Peculiar Velocity Field
    OBSERVATIONAL STUDIES OF THE GALAXY PECULIAR VELOCITY FIELD by Philip Andrew James Astrophysics Group Blackett Laboratory Imperial College of Science, Technology and Medicine London SW7 2BZ A thesis submitted for the degree of Doctor of Philosophy of the University of London and for the Diploma of Imperial College November 1988 1 ABSTRACT This thesis describes two observational studies of the peculiar velocity field of galaxies over scales of 50-100 Jr1 Mpc, and the consequences of these measurements for cosmological theories. An introduction is given to observational cosmology, emphasising the crucial questions of the nature of the dark matter and the formation of structure. The principal cosmological models are discussed, and the role of observations in developing these models is stressed. Consideration is given to those observations that are likely to prove good discriminators between the competing models, particular emphasis being given to studies of the coherent velocities of samples of galaxies. The first new study presented here uses optical photometry and redshifts, from the literature, for First Ranked Cluster Galaxies (FRCG’s). These galaxies are excellent standard candles, and thus ideal for peculiar velocity studies. A simple one­ dimensional analysis detects no relative motion between the Local Group of galaxies and 60 FRCG’s with redshifts of up to 15000 kms-1. This is shown to imply a streaming motion of the cluster galaxies of at least 600 kms_1 relative to the CBR. The second observational study is a reanalysis of the Rubin et al. (1976a,b) sample of Sc galaxies. Near-IR photometry is used in our reanalysis to minimise the effects of extinction and to facilitate the use of luminosity indicators in reducing the effects of selection biases.
    [Show full text]
  • Emissão Infra - Vermelha De Galáxias Iras
    UNIVERSIDADE FEDERAL DO RIO GRANDE DO SUL INSTITUTO DE FÍSICA EMISSÃO INFRA - VERMELHA DE GALÁXIAS IRAS Charles José Bonatto Tese realizada sob a orientação da Dra. Miriani G. Pastoriza e apresentada ao Instituto de Física da UFRGS, em preenchi- mento parcial dos requisitos para a obtenção do título de Doutor em Física. Porto Alegre 1992 *Trabalho financiado pelo Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq). Aos meus pais, irmãos e cunhados. Agradecimentos À Miriani Pastoriza por sua orientação e confiança; À Sebastian Lípari por ter fornecido as observações de CASLEO; A todo o pessoal do Departamento de Astronomia, pelos bons momentos que têm sido proporcionados; Ao pessoal da Biblioteca, em especial à Zuleika e à Ana; A todas as pessoas que direta ou indiretamente contribuíram para este trabalho; Ao CNPq, pelo financiamento deste trabalho; À FAPERGS, pelo apoio financeiro em um dos turnos em Tololo. Resumo Galáxias ativas emitem fortemente no infra-vermelho. Grãos de poeira, aquecidos por fótons Ultra-Violeta e ópticos absorvem estes fótons e os re-emitem no infra-vermelho. Atualmente, esta é a interpretação mais provável para esta emissão no infra-vermelho. Neste trabalho, desenvolvemos um modelo para a emissão e distribuição espacial dos graõs de poeira, incluindo a contribuição de uma lei-de-potência. Usamos galáxias com observações no óptico e no infra-vermelho, separando-as em Seyfert tipo 1 e 2, para analisar as relações entre luminosidades de linhas de emissão no óptico e a luminosidade no infra-vermelho (LIR). Contando o número de galáxias com L r.. dentro de um determinado intervalo, mostramos que as distribuições de LIR de Seyferts tipo 1 e 2 são quase idênticas.
    [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]
  • Synapses of Active Galactic Nuclei: Comparing X-Ray and Optical Classifications Using Artificial Neural Networks?
    A&A 567, A92 (2014) Astronomy DOI: 10.1051/0004-6361/201322592 & c ESO 2014 Astrophysics Synapses of active galactic nuclei: Comparing X-ray and optical classifications using artificial neural networks? O. González-Martín1;2;??, D. Díaz-González3, J. A. Acosta-Pulido1;2, J. Masegosa4, I. E. Papadakis5;6, J. M. Rodríguez-Espinosa1;2, I. Márquez4, and L. Hernández-García4 1 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna (ULL), 38205 La Laguna, Spain 3 Shidix Technologies, 38320, La Laguna, Spain 4 Instituto de Astrofísica de Andalucía, CSIC, C/ Glorieta de la Astronomía s/n, 18005 Granada, Spain 5 Physics Department, University of Crete, PO Box 2208, 710 03 Heraklion, Crete, Greece 6 IESL, Foundation for Research and Technology, 711 10 Heraklion, Crete, Greece Received 2 September 2013 / Accepted 3 April 2014 ABSTRACT Context. Many classes of active galactic nuclei (AGN) have been defined entirely through optical wavelengths, while the X-ray spectra have been very useful to investigate their inner regions. However, optical and X-ray results show many discrepancies that have not been fully understood yet. Aims. The main purpose of the present paper is to study the synapses (i.e., connections) between X-ray and optical AGN classifications. Methods. For the first time, the newly implemented efluxer task allowed us to analyse broad band X-ray spectra of a sample of emission-line nuclei without any prior spectral fitting. Our sample comprises 162 spectra observed with XMM-Newton/pn of 90 lo- cal emission line nuclei in the Palomar sample.
    [Show full text]
  • (Ap) Mag Size Distance Rise Transit Set Gal NGC 6217 Arp 185 Umi
    Herschel 400 Observing List, evening of 2015 Oct 15 at Cleveland, Ohio Sunset 17:49, Twilight ends 19:18, Twilight begins 05:07, Sunrise 06:36, Moon rise 09:51, Moon set 19:35 Completely dark from 19:35 to 05:07. Waxing Crescent Moon. All times local (EST). Listing All Classes visible above the perfect horizon and in twilight or moonlight before 23:59. Cls Primary ID Alternate ID Con RA (Ap) Dec (Ap) Mag Size Distance Rise Transit Set Gal NGC 6217 Arp 185 UMi 16h31m48.9s +78°10'18" 11.9 2.6'x 2.1' - 15:22 - Gal NGC 2655 Arp 225 Cam 08h57m35.6s +78°09'22" 11 4.5'x 2.8' - 7:46 - Gal NGC 3147 MCG 12-10-25 Dra 10h18m08.0s +73°19'01" 11.3 4.1'x 3.5' - 9:06 - PNe NGC 40 PN G120.0+09.8 Cep 00h13m59.3s +72°36'43" 10.7 1.0' 3700 ly - 23:03 - Gal NGC 2985 MCG 12-10-6 UMa 09h51m42.0s +72°12'01" 11.2 3.8'x 3.1' - 8:39 - Gal Cigar Galaxy M 82 UMa 09h57m06.5s +69°35'59" 9 9.3'x 4.4' 12.0 Mly - 8:45 - Gal NGC 1961 Arp 184 Cam 05h43m51.6s +69°22'44" 11.8 4.1'x 2.9' 180.0 Mly - 4:32 - Gal NGC 2787 MCG 12-9-39 UMa 09h20m40.5s +69°07'51" 11.6 3.2'x 1.8' - 8:09 - Gal NGC 3077 MCG 12-10-17 UMa 10h04m31.3s +68°39'09" 10.6 5.1'x 4.2' 12.0 Mly - 8:52 - Gal NGC 2976 MCG 11-12-25 UMa 09h48m29.2s +67°50'21" 10.8 6.0'x 3.1' 15.0 Mly - 8:36 - PNe Cat's Eye Nebula NGC 6543 Dra 17h58m31.7s +66°38'25" 8.3 22" 4400 ly - 16:49 - Open NGC 7142 Collinder 442 Cep 21h45m34.2s +65°51'16" 10 12.0' 5500 ly - 20:35 - Gal NGC 2403 MCG 11-10-7 Cam 07h38m20.9s +65°33'36" 8.8 20.0'x 10.0' 11.0 Mly - 6:26 - Open NGC 637 Collinder 17 Cas 01h44m15.4s +64°07'07" 7.3 3.0' 7000 ly - 0:33
    [Show full text]
  • 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]
  • A Complete Redshift Survey to the Zwicky Catalog Limit in a 2-Hour by 15-Degree Region Around 3C
    A Complete Redshift Survey to the Zwicky Catalog Limit in a 2h × 15◦ Region Around 3C 273 Norman A. Grogin, Margaret J. Geller, and John P. Huchra Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 E-mail: ngrogin, mgeller, [email protected] ABSTRACT We compile 1113 redshifts (648 new measurements, 465 from the literature) for Zwicky catalogue galaxies in the region (−3◦.5 ≤ δ ≤ 8◦.5, 11h.5 ≤ α ≤ 13h.5). We include redshifts for 114 component objects in 78 Zwicky catalogue multiplets. The redshift survey in this region is 99.5% complete to the Zwicky catalogue limit, mZw = 15.7. It is 99.9% complete to mZw = 15.5, the CfA Redshift Survey (CfA2) magnitude limit. The survey region is adjacent to the northern portion of CfA2, overlaps the northernmost slice of the Las Campanas Redshift Survey, includes the southern extent of the Virgo Cluster, and is roughly centered on the QSO 3C 273. As in other portions of the Zwicky catalogue, bright and faint galaxies trace the same large-scale structure. Subject headings: cosmology: observations — galaxies: distances and redshifts — galaxies: interactions 1. Introduction arXiv:astro-ph/9807067v1 7 Jul 1998 The Center for Astrophysics Redshift Survey (hereafter CfA2, Geller & Huchra 1989) of galaxies from Zwicky’s Catalogue of Galaxies and Clusters of Galaxies (Zwicky et al. 1961–1968, hereafter CGCG) still remains one of the best re- sources for the study of the nearby galaxy distribution. In a recent paper (Gro- gin & Geller 1998), we used CfA2 to investigate the connection between local −1 (cz ∼< 10000 km s ) Lyman-alpha absorption systems observed with HST (Bah- call et al.
    [Show full text]
  • CO Observations Towards a Sample of Nearby Galaxies
    RAA 2015 Vol. 15 No. 6, 785–801 doi: 10.1088/1674–4527/15/6/002 Research in http://www.raa-journal.org http://www.iop.org/journals/raa Astronomy and Astrophysics CO observations towards a sample of nearby galaxies Fa-Cheng Li1,2, Yuan-Wei Wu1 and Ye Xu1 1 Purple Mountain Observatory, & Key Laboratory for Radio Astronomy, Chinese Academy of Sciences, Nanjing 210008, China; [email protected] 2 University of Chinese Academy of Sciences, Beijing 100049, China Received 2013 November 26; accepted 2014 November 13 Abstract We have simultaneously observed 12CO, 13CO and C18O (J = 1 − 0) rotational transitions in the centers of a sample of 58 nearby spiral galaxies using the 13.7-m millimeter-wave telescope administered by Purple Mountain Observatory. Forty-two galaxies were detected in 13CO emission, but there was a null detection for C18O emission with a σ upper limit of 2 mK. The central beam ratios, R, of 12CO and 13CO range mostly from 5 to 13, with an average value of 8.1±4.2, which is slightly lower than previous estimates for normal galaxies. Clear correlations are found between 12CO and 13CO luminosities. An average X factor of 1.44 ± 0.84 × 1020 cm−2 (K km s−1)−1 is slightly lower than that in the Milky Way. Key words: galaxies: ISM — molecules: galaxies — millimeter lines: ISM — star formation: ISM 1 INTRODUCTION Molecular hydrogen, H2, constitutes a dominant part of molecular clouds in the interstellar medium in galaxies and is most closely related to star formation. The current method of studying molecular clouds in external galaxies involves the observation of rotational transitions of carbon monoxide, CO.
    [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]
  • Arxiv:1207.4189V1 [Astro-Ph.CO] 17 Jul 2012 N a Osdrtrefnaetlpyia Parame- Physical Fundamental Mass Three Alternatively, Ters: Consider Color
    The Astrophysical Journal Supplement Series, in press, 17 July 2012 A Preprint typeset using LTEX style emulateapj v. 5/2/11 ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED Aaron J. Romanowsky1, S. Michael Fall2 1University of California Observatories, Santa Cruz, CA 95064, USA 2Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA The Astrophysical Journal Supplement Series, in press, 17 July 2012 ABSTRACT Motivated by a new wave of kinematical tracers in the outer regions of early-type galaxies (ellipticals and lenticulars), we re-examine the role of angular momentum in galaxies of all types. We present new methods for quantifying the specific angular momentum j, focusing mainly on the more challenging case of early-type galaxies, in order to derive firm empirical relations between stellar j⋆ and mass M⋆ (thus extending the work by Fall 1983). We carry out detailed analyses of eight galaxies with kinematical data extending as far out as ten effective radii, and find that data at two effective radii are generally sufficient to estimate total j⋆ reliably. Our results contravene suggestions that ellipticals could harbor large reservoirs of hidden j⋆ in their outer regions owing to angular momentum transport in major mergers. We then carry out a comprehensive analysis of extended kinematic data from the literature for a sample of 100 nearby bright galaxies of all types, placing them on a diagram of ∼ j⋆ versus M⋆. The ellipticals and spirals form two parallel j⋆–M⋆ tracks, with log-slopes of 0.6, which for the spirals is closely related to the Tully-Fisher relation, but for the ellipticals derives from∼ a remarkable conspiracy between masses, sizes, and rotation velocities.
    [Show full text]