DOCSLIB.ORG

The Bulgeless Seyfert/LINER Galaxy NGC 3367: Disk, Bar

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The Bulgeless Seyfert/LINER Galaxy NGC 3367: Disk, Bar The Bulgeless Seyfert/LINER Galaxy NGC 3367: Disk, Bar, Lopsidedness and Environment1 H. M. Hern´andez-Toledo2,a, M. Cano-D´ıaza,b, O. Valenzuelaa, I. Pueraric, J. A. Garc´ıa-Barretoa, E. Moreno-D´ıaza, H. Bravo-Alfarod aInstituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, Apartado Postal 70-264, Mexico D.F., 04510, Mexico bINAF-Osservatorio Astronomico di Roma, via di Frascati 33, 00040, Monte Porzio Catone, Italy cInstituto Nacional de Astrof´ısica, Optica´ y Electr´onica, Calle Luis Enrique Erro 1, 72840, Sta. Mar´ıa Tonantzintla, Puebla, Mexico dDepartamento de Astronom´ıa, Universidad de Guanajuato, Apdo. Postal 144, Guanajuato 36000, Mexico ABSTRACT NGC 3367 is a nearby isolated active galaxy that shows a radio jet, a strong bar and evidence of lopsidedness. We present a quantitative analysis of the stellar and gaseous structure of the galaxy disk and a search for evidence of recent interaction based on new UBV RI Hα and JHK images and on archival Hα Fabry-Perot and HI VLA data. From a coupled 1D/2D GALFIT bulge/bar/disk decomposition an (B/D ∼ 0.07-0.1) exponential pseudobulge is inferred in all the max observed bands. A NIR estimate of the bar strength <QT (R) > = 0.44 places NGC 3367 bar among the strongest ones. The asymmetry properties were studied using (1) optical and NIR CAS indexes (2) the stellar (NIR) and gaseous (Hα, HI) A1 Fourier mode amplitudes and (3) the HI integrated profile and HI mean intensity distribution. While the average stellar component shows asymmetry values close to the average found in the Local Universe for isolated galaxies, the young stellar component and gas values are largely decoupled showing significantly larger A1 mode amplitudes suggesting that the gas has been recently perturbed. NGC 3367 is devoided of HI gas in the central regions where a significant amount of molecular CO gas exists instead. −2 Our search for (1) faint stellar structures in the outer regions (up to µR ∼ 26 mag arcsec ), (2) (Hα) star-forming satellite galaxies and (3) regions with different colors (stellar populations) along the disk all failed. Such an absence is interpreted using recent numerical simulations to constrain a tidal event with an LMC like galaxy to some dynamical times in the past or to a current very low mass, gas rich accretion. We conclude that a cold accretion mode (gas and small/dark galaxies) may be responsible of the nuclear activity and peculiar (young stars and arXiv:1104.3622v4 [astro-ph.CO] 26 Apr 2011 gas) morphology regardless of the highly isolated environment. Black hole growth in bulgeless galaxies may be triggered by cosmic smooth mass accretion. Subject headings: Galaxies: individual – Galaxies: structure – Galaxies: bars – Galaxies: photometry – Galaxies: interactions – Galaxies: morphology – Galaxies: general 1. Introduction 1Based on data obtained at the 0.84m, 1.5m and 2.1m telescopes of the Observatorio Astron´omico Nacional, San NGC 3367 is a nearby barred galaxy that is Pedro M´artir operated by the Instituto de Astronom´ıa, classified as SB(rs)c in the Third Reference Cata- Universidad Nacional Aut´onoma de M´exico. log of Bright Galaxies (de Vaucouleurs et al. 1991, hereafter RC3) and as Sy 2-like, HII in V´eron- Cetty & V´eron (1986). MIR Spitzer observations 1 of NGC 3367 reveal the presence of [Ne v] lines at measurements as constraints to the recent dynam- 14.3µm and 24.3µm with X-ray luminosity domi- ical history in NGC 3367. Specifically, a descrip- nated by a power law with 2-10 keV luminosities tion of observations and the techniques used in the of 2.0 ×1040erg s−1 (McAlpine et al. 2011). NGC data reduction are briefly described in Section 2. 3367 is located in the field of the Leo Group but In Section 3 we present a brief summary of the it belongs to the background based on its opti- main morphological features found in the optical −1 cal velocity of vo = 2998 km s and the mean and NIR images. A surface photometry analysis velocity ofthe Leo I Group = 900 km s−1 (Fergu- is carried out in Section 4, including (i) an analy- son and Sandage 1990; Stocke et al. 1991; Tonry sis of the surface brightness and color profiles, (ii) et al. 2001). The closest candidate for a galaxy a coupled 1D-2D bulge/disk and bulge/bar/disk companion is NGC 3391 at a projected distance of decomposition into S´ersic, Exponential and Fer- ∼ 563 kpc or 18 optical diameters away (Garc´ıa- rer components. Section 5 presents different bar Barreto et al. 2003) and a recent search for iso- properties like ISM shocks based on the dust lane lated galaxies in the local Universe based on the geometry revealed by a B − I color map, a quan- SDSS has also confirmed that NGC 3367 is an iso- tification of the bar strength and length, and a lated galaxy (Hern´andez-Toledo et al. 2010). The brief discussion of the bar nature in terms of the optical appearance of NGC 3367 is dominated by a Athanassoula & Misiriotis (2002) models. In Sec- bright bar and an apparent large-scale asymmetry tion 6 Lopsidedness is reviewed from various es- or lopsidedness to the southwest side. timators, namely, the Concentration-Asymmetry- Radio observations in NGC 3367 reveal a bipo- Clumpiness (hereafter CAS) parameters in the op- lar synchrotron outflow from the nucleus and two tical and NIR bands, the m = 0 − 2 Fourier NIR large lobes with a total projected extent on the and Hα amplitudes and the VLA HI asymmetry sky (from NE-to-SW) of 12 kpc, resembling a ra- from the moment 0 distribution and the corre- dio galaxy. The axis of the ejected outflow is sponding HI line profile. In Section 7 we look highly inclined with respect to the axis of rotation for (i) evidence of low surface brightness features of the disk (Garc´ıa-Barreto et al. 1998; Garc´ıa- likely related to a tidal origin and (ii) the presence Barreto, Franco & Rudnick 2002). Single-dish HI of recent galaxy accretion events or satellite com- 9 content of MHI ∼ 7 × 10 M⊙ has been reported panions in the observed colors. Section 8 presents for this galaxy (Huchtmeier & Richter 1989) and a general discussion on the origin of the disk Lop- a high fraction of molecular gas has been found sidedness. We use Fabry-Perot Hα and HI VLA mostly concentrated in the central 27′′ (r=5.7 kpc) data to discuss possible evidence of anisotropic gas M(H2) = 2.7 × 109M⊙ (Garc´ıa-Barreto et al. accretion and its possible connection to the AGN 2005). NGC 3367 also shows weak thermal radio activity in NGC 3367. Finally, our summary and continuum emission (at 4.5” angular resolution) concluding remarks are presented in Section 9. A −1 −1 extended throughout the disk (Garc´ıa-Barreto et distance of 43.6 Mpc (Ho = 75 km s Mpc ) is al. 1998) and Hα Fabry-Perot observations in- adopted for NGC 3367 (Tully 1988), resulting in −1 dicate that its rotation axis lies projected on the a linear scale of 210 pc arcsec . disk at a P.A. of 141◦, the N side of that projected line being closer to the observer (Garc´ıa-Barreto 2. Observations and Data Reduction & Rosado 2001). The optical UBV RI observations were carried Despite that several properties of NGC 3367 out at the 0.84m telescope of the Observatorio As- somehow resemble a gravitational interacting sys- tron´omico Nacional at San Pedro M´artir (OAN- tem with another galaxy, there is yet no support- SPM), Baja California, M´exico, with a Site1 CCD ing evidence. This is the first paper of a series detector yielding a total field of view of 7.2 x 7.2 where we present our multi-wavelength data and arcmin and typical seeing FWHM values of 1.8 discuss some alternatives to the origin of the ob- arcsec. A detailed description of the optical ob- served morphology and asymmetries. Our paper is servations and the standard data reduction within split into two general parts; one describing the ob- servations and the estimate of the galaxy parame- ters and the second discussing the interpretation of 2 the IRAF platform 3 can be found in Garc´ıa- then subtracted from the original image to en- Barreto et al. (2007). The routines under Space hance both internal and external structures in the Telescope Science Data Analysis System (STS- form of star forming regions, structures embedded DAS) were used in the reduction and analysis of into dusty regions or faint outer details of partic- both the optical and near-IR data. In this pa- ular interest for our discussion. per a further processing of the images in 2 × 2 The bluer bands highlight a sharp semi-circular binning mode was applied to have a pixel scale outline at the N-W-S direction. This structure of 0.85 arcsec/pix, similar to that in the Near-IR presents a complex pattern of arms at a radius observations. of about 50 arcsec (10 kpc) from the center. The The Near-IR observations were carried out us- arms in the inner region almost coalesce to form an ing the CAMILA instrument (Cruz-Gonz´alez et internal ring. Some bright HII regions are strung al. 1994) at the OAN-SPM 2.1m telescope. The along the inner parts of two major arms that begin CAMILA instrument uses a NICMOS 3 detector at the ends of the bar, these arms experiencing of 256 x 256 pixel format.
Load more

Recommended publications
  • 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]
  • April 14 2018 7:00Pm at the April 2018 Herrett Center for Arts & Science College of Southern Idaho
    Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Tim Frazier Saturday, April 14th 2018 April 2018 7:00pm at the Herrett Center for Arts & Science College of Southern Idaho. It really is beginning to feel like spring. The weather is more moderate and there will be, hopefully, clearer skies. (I write this with some trepidation as I don’t want to jinx Public Star Party Follows at the it in a manner similar to buying new equipment will ensure at least two weeks of Centennial Observatory cloudy weather.) Along with the season comes some great spring viewing. Leo is high overhead in the early evening with its compliment of galaxies as is Coma Club Officers Berenices and Virgo with that dense cluster of extragalactic objects. Tim Frazier, President One of my first forays into the Coma-Virgo cluster was in the early 1960’s with my [email protected] new 4 ¼ inch f/10 reflector and my first star chart, the epoch 1960 version of Norton’s Star Atlas. I figured from the maps I couldn’t miss seeing something since Robert Mayer, Vice President there were so many so closely packed. That became the real problem as they all [email protected] appeared as fuzzy spots and the maps were not detailed enough to distinguish one galaxy from another. I still have that atlas as it was a precious Christmas gift from Gary Leavitt, Secretary my grandparents but now I use better maps, larger scopes and GOTO to make sure [email protected] it is M84 or M86.
    [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]
  • Nuclear Activity in Circumnuclear Ring Galaxies
    International Journal of Astronomy and Astrophysics, 2016, 6, 219-235 Published Online September 2016 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2016.63018 Nuclear Activity in Circumnuclear Ring Galaxies María P. Agüero1, Rubén J. Díaz2,3, Horacio Dottori4 1Observatorio Astronómico de Córdoba, UNCand CONICET, Córdoba, Argentina 2ICATE, CONICET, San Juan, Argentina 3Gemini Observatory, La Serena, Chile 4Instituto de Física, UFRGS, Porto Alegre, Brazil Received 23 May 2016; accepted 26 July 2016; published 29 July 2016 Copyright © 2016 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75% of the hosts), with a bar (44% weak, 37% strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem
    [Show full text]
  • The (Black Hole Mass)-(Host Spheroid Luminosity) Relation at High and Low
    Draft version July 22, 2018 Preprint typeset using LATEX style emulateapj v. 03/07/07 THE (BLACK HOLE MASS)–(HOST SPHEROID LUMINOSITY) RELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES Alister W. Graham1 and Nicholas Scott Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia. Draft version July 22, 2018 ABSTRACT From a sample of 72 galaxies with reliable supermassive black hole masses Mbh, we derive the Mbh– (host spheroid luminosity, L) relation for i) the subsample of 24 core-S´ersic galaxies with partially depleted cores, and ii) the remaining subsample of 48 S´ersic galaxies. Using Ks-band Two Micron 1.10±0.20 All Sky Survey data, we find the near-linear relation Mbh L for the core-S´ersic spheroids ∝ Ks thought to be built in additive dry merger events, while M L2.73±0.55 for the S´ersic spheroids built bh Ks from gas-rich processes. After converting literature B-band∝ disk galaxy magnitudes into inclination- and dust-corrected bulge magnitudes, via a useful new equation presented herein, we obtain a similar result. Unlike with the Mbh–(velocity dispersion) diagram, which is also updated here using the same galaxy sample, it remains unknown whether barred and non-barred S´ersic galaxies are offset from each other in the Mbh–L diagram. While black hole feedback has typically been invoked to explain what was previously thought to be a nearly constant M /M mass ratio of 0.2%, we advocate that the near-linear M – bh Spheroid ∼ bh L and Mbh–MSpheroid relations observed at high masses may have instead largely arisen from the additive dry merging of galaxies.
    [Show full text]
  • Type II Supernovae As Probes of Environment Metallicity: Observations of Host H II Regions J
    A&A 589, A110 (2016) Astronomy DOI: 10.1051/0004-6361/201527691 & c ESO 2016 Astrophysics Type II supernovae as probes of environment metallicity: observations of host H II regions J. P. Anderson1, C. P. Gutiérrez1; 2; 3, L. Dessart4, M. Hamuy3; 2, L. Galbany2; 3, N. I. Morrell5, M. D. Stritzinger6, M. M. Phillips5, G. Folatelli7, H. M. J. Boffin1, T. de Jaeger2; 3, H. Kuncarayakti2; 3, and J. L. Prieto8; 2 1 European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile e-mail: [email protected] 2 Millennium Institute of Astrophysics, Casilla 36-D, Santiago, Chile 3 Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile 4 Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Boulevard de l’Observatoire, CS 34229, 06304 Nice Cedex 4, France 5 Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile 6 Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark 7 Instituto de Astrofísica de La Plata, Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, CONICET, Paseo del Bosque S/N, B1900FWA, La Plata, Argentina 8 Núcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile Received 3 November 2015 / Accepted 28 January 2016 ABSTRACT Context. Spectral modelling of type II supernova atmospheres indicates a clear dependence of metal line strengths on progenitor metallicity. This dependence motivates further work to evaluate the accuracy with which these supernovae can be used as environment metallicity indicators. Aims.
    [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]
  • 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]
  • Stellar Population in LLAGN. II: STIS Observations
    Stellar Population in LLAGN.II: STIS observations 1 Rosa M. Gonz´alez Delgado1, Roberto Cid Fernandes2, Enrique P´erez1, Lucimara P. Martins3,7, Thaisa Storchi-Bergmann4, Henrique Schmitt5,8, Timothy Heckman6,9, & Claus Leitherer3 (1) Instituto de Astrof´ısica de Andalucia (CSIC), P.O. Box 3004, 18080 Granada, Spain ([email protected]; [email protected]) (2) Depto. de F´ısica-CFM, Universidade Federal de Santa Catarina, C.P. 476, 88040-900, Florian´opolis, SC, Brazil ([email protected]) (3) Space Telescope Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ([email protected]; [email protected]) (4) National Radio Astronomy Observatory, PO Box 0, Socorro, NM 87801 ([email protected]) (5) Instituto de F´ısica, Universidad Federal do Rio Grande do Sul, C.P. 15001, 91501-970, Poto Alegre, RS, Brazil ([email protected]) (6) Department of Physics & Astronomy, JHU, Baltimore, MD 21218 ([email protected]) (7) Intituto de Astronom´ıa, Geof´ısica e Ciencias Atmosf´ericas, 05508-900 Sao Paulo, Brazil ABSTRACT arXiv:astro-ph/0401414v1 21 Jan 2004 We present a study of the stellar population in Low Luminosity Active Galac- tic Nuclei (LLAGN). Our goal is to search for spectroscopic signatures of young and intermediate age stars, and to investigate their relationship with the ioniza- tion mechanism in LLAGN. The method used is based on the stellar population synthesis of the optical continuum of the innermost (20-100 pc) regions in these galaxies. For this purpose, we have collected high spatial resolution optical (2900- 5700 A)˚ STIS spectra of 28 nearby LLAGN that are available in the Hubble Space Telescope archive.
    [Show full text]
  • Fabry Perot Halpha Observations of the Barred Spiral NGC 3367
    Fabry Perot Hα observations of the Barred Spiral NGC 3367 J.Antonio Garc´ıa-Barreto and M. Rosado Instituto de Astronom´ıa, Universidad Nacional Aut´onoma de M´exico, Apartado Postal 70-264, M´exico D.F. 04510 M´exico Received ; accepted January 22, 2001 arXiv:astro-ph/0101394v1 22 Jan 2001 –2– ABSTRACT We report the gross properties of the velocity field of the barred spiral galaxy NGC 3367. We obtained the following values : inclination with respect to the plane of the sky, i = 30; position angle (P.A.) of receding semi major axis, ◦ −1 P.A.= 51 and systemic velocity, Vsys = 3032 km s . Large velocity dispersion are observed of up to 120 km s−1 in the nuclear region, of up to 70 km s−1 near the eastern bright sources just beyond the edge of the stellar bar where three spiral arms seem to start and in the western bright sources at about 10 kpc. Deviations from normal circular velocities are observed from all the disk but mainly from the semi circle formed by the string of south western Hα sources. 11 An estimate of the dynamical mass is Mdyn =2 × 10 M⊙. Subject headings: galaxies: individual NGC 3367 — galaxies: kinematics and dynamics — galaxies: Hα emission — galaxies: structure — –3– 1. Introduction NGC 3367 is an SBc barred spiral galaxy considered isolated at a distance of 43.6 Mpc −1 −1 behind the Leo Spur group of galaxies (i.e. using H0 = 75 km s Mpc Tully 1988), with a distant neighbor NGC 3419 at 900 ± 100 kpc away.
    [Show full text]
  • 1989Aj 98. .7663 the Astronomical Journal
    .7663 THE ASTRONOMICAL JOURNAL VOLUME 98, NUMBER 3 SEPTEMBER 1989 98. THE IRAS BRIGHT GALAXY SAMPLE. IV. COMPLETE IRAS OBSERVATIONS B. T. Soifer, L. Boehmer, G. Neugebauer, and D. B. Sanders Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, California 91125 1989AJ Received 15 March 1989; revised 15 May 1989 ABSTRACT Total flux densities, peak flux densities, and spatial extents, are reported at 12, 25, 60, and 100 /¿m for all sources in the IRAS Bright Galaxy Sample. This sample represents the brightest examples of galaxies selected by a strictly infrared flux-density criterion, and as such presents the most complete description of the infrared properties of infrared bright galaxies observed in the IRAS survey. Data for 330 galaxies are reported here, with 313 galaxies having 60 fim flux densities >5.24 Jy, the completeness limit of this revised Bright Galaxy sample. At 12 /¿m, 300 of the 313 galaxies are detected, while at 25 pm, 312 of the 313 are detected. At 100 pm, all 313 galaxies are detected. The relationships between number counts and flux density show that the Bright Galaxy sample contains significant subsamples of galaxies that are complete to 0.8, 0.8, and 16 Jy at 12, 25, and 100 pm, respectively. These cutoffs are determined by the 60 pm selection criterion and the distribution of infrared colors of infrared bright galaxies. The galaxies in the Bright Galaxy sample show significant ranges in all parameters measured by IRAS. All correla- tions that are found show significant dispersion, so that no single measured parameter uniquely defines a galaxy’s infrared properties.
    [Show full text]