47 Tuc, 287 Abundance Gradients, 3, 523 Angular Momentum, 187, 513
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Near-Infrared Luminosity Relations and Dust Colors L
A&A 578, A47 (2015) Astronomy DOI: 10.1051/0004-6361/201525817 & c ESO 2015 Astrophysics Obscuration in active galactic nuclei: near-infrared luminosity relations and dust colors L. Burtscher1, G. Orban de Xivry1, R. I. Davies1, A. Janssen1, D. Lutz1, D. Rosario1, A. Contursi1, R. Genzel1, J. Graciá-Carpio1, M.-Y. Lin1, A. Schnorr-Müller1, A. Sternberg2, E. Sturm1, and L. Tacconi1 1 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Gießenbachstr., 85741 Garching, Germany e-mail: [email protected] 2 Raymond and Beverly Sackler School of Physics & Astronomy, Tel Aviv University, 69978 Ramat Aviv, Israel Received 5 February 2015 / Accepted 5 April 2015 ABSTRACT We combine two approaches to isolate the AGN luminosity at near-IR wavelengths and relate the near-IR pure AGN luminosity to other tracers of the AGN. Using integral-field spectroscopic data of an archival sample of 51 local AGNs, we estimate the fraction of non-stellar light by comparing the nuclear equivalent width of the stellar 2.3 µm CO absorption feature with the intrinsic value for each galaxy. We compare this fraction to that derived from a spectral decomposition of the integrated light in the central arcsecond and find them to be consistent with each other. Using our estimates of the near-IR AGN light, we find a strong correlation with presumably isotropic AGN tracers. We show that a significant offset exists between type 1 and type 2 sources in the sense that type 1 MIR X sources are 7 (10) times brighter in the near-IR at log LAGN = 42.5 (log LAGN = 42.5). -
N6l0-Aistralian Observatory
^^—^^r N6L0-AISTRALIAN OBSERVATORY GAS DYNAMICS IN BARRED SPIRALS, II: NGC 7496 AND 289 V.D. Pence and C.P. BlackMn AAO PP 194 * Suonitted to: Mon.Not.R.astr.Soc. Distribution date: February, 1984 P.O. BOX 296. EPPING. N.S.W.. 2121 PHONE 868-1666. TELEX ASTRO 26230 „. *u~ - .*.SÄ._TNW. - Afto-<?(*-- ^M GAS DYNAMICS IN BARRED SPIRALS, II: NGC 7496 AND 289 W.D.Pence. Anglo-Australian Observatory. P.O. Box 296. Epplng. NSW. Australia. C.P.Blactanan. Department of Astronomy. Edinburgh University. Received t SUMMAKT - The gas velocity fields in the barred spiral galaxies NGC 7496 and 289 have been measured by means of long-slit spectra obtained with the Anglo-Australian Telescope. Pronounced deviations fro« circular motion of the type predicted by recent theoretical mooels are seen in NGC 74961 the isovelocity contours are distorted into a characteristic S-shaped pattern and there is a large velocity gradient across the bar. The velocity field is virtually identical to that of a previously observed barred spiral, NGC 5383 for which a number of models have been published. The nuclear [OUI] emission lines are very asymmetric with a wing extending to about 1000 km s-1 to the blue of the systemic velocity; this wing is only faintly seen in the Balmer lines. NGC 289 has a much smaller bar *nd consequently the noncircular motions are less pronounced. The most obvious effect is that the Xinematic major and minor axes are not perpendicular which is a signature of oval distortions. Both galaxies have a mass (within the 10 outermost velocity measurement) of 9 x iO M0 and M/Lß » 6. -
Southern Arp - AM # Order
Southern Arp - AM # Order A B C D E F G H I J 1 AM # Constellation Object Name RA DEC Mag. Size Uranom. Uranom. Millenium 2 1st Ed. 2nd Ed. 3 AM 0003-414 Phoenix ESO 293-G034 00h06m19.9s -41d30m00s 13.7 3.2 x 1.0 386 177 430 Vol I 4 AM 0006-340 Sculptor NGC 10 00h08m34.5s -33d51m30s 13.3 2.4 x 1.2 350 159 410 Vol I 5 AM 0007-251 Sculptor NGC 24 00h09m56.5s -24d57m47s 12.4 5.8 x 1.3 305 141 366 Vol I 6 AM 0011-232 Cetus NGC 45 00h14m04.0s -23d10m55s 11.6 8.5 x 5.9 305 141 366 Vol I 7 AM 0027-333 Sculptor NGC 134 00h30m22.0s -33d14m39s 11.4 8.5 x 2.0 351 159 409 Vol I 8 AM 0029-643 Tucana ESO 079- G003 00h32m02.2s -64d15m12s 12.6 2.7 x 0.4 440 204 409 Vol I 9 AM 0031-280B Sculptor NGC 150 00h34m15.5s -27d48m13s 12 3.9 x 1.9 306 141 387 Vol I 10 AM 0031-320 Sculptor NGC 148 00h34m15.5s -31d47m10s 13.3 2 x 0.8 351 159 387 Vol I 11 AM 0033-253 Sculptor IC 1558 00h35m47.1s -25d22m28s 12.6 3.4 x 2.5 306 141 365 Vol I 12 AM 0041-502 Phoenix NGC 238 00h43m25.7s -50d10m58s 13.1 1.9 x 1.6 417 177 449 Vol I 13 AM 0045-314 Sculptor NGC 254 00h47m27.6s -31d25m18s 12.6 2.5 x 1.5 351 176 386 Vol I 14 AM 0050-312 Sculptor NGC 289 00h52m42.3s -31d12m21s 11.7 5.1 x 3.6 351 176 386 Vol I 15 AM 0052-375 Sculptor NGC 300 00h54m53.5s -37d41m04s 9 22 x 16 351 176 408 Vol I 16 AM 0106-803 Hydrus ESO 013- G012 01h07m02.2s -80d18m28s 13.6 2.8 x 0.9 460 214 509 Vol I 17 AM 0105-471 Phoenix IC 1625 01h07m42.6s -46d54m27s 12.9 1.7 x 1.2 387 191 448 Vol I 18 AM 0108-302 Sculptor NGC 418 01h10m35.6s -30d13m17s 13.1 2 x 1.7 352 176 385 Vol I 19 AM 0110-583 Hydrus NGC -
The NICMOS Snapshot Survey of Nearby Galaxies
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server The NICMOS snapshot survey of nearby galaxies T. B¨oker1, D. Calzetti, W. Sparks, D. Axon1, L. E. Bergeron, H. Bushouse, L. Colina1, D. Daou, D. Gilmore, S. Holfeltz, J. MacKenty, L. Mazzuca, B. Monroe, J. Najita, K. Noll, A. Nota1,C. Ritchie, A. Schultz, M. Sosey, A. Storrs, A. Suchkov (the STScI NICMOS group) Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A. ABSTRACT We present “snapshot” observations with the NearInfrared Camera and MultiObject Spectrometer (NICMOS) on board the Hubble Space Telescope (HST) of 94 nearby galaxies from the Revised Shapley Ames Catalog. Images with 0.200 resolution were obtained in two filters, a broad-band continuum filter (F160W, roughly equivalent to the H-band) and a narrow band filter centered on the Pa α line (F187N or F190N, depending on the galaxy redshift) with the 5100 5100 field of view of the NICMOS camera 3. A first- order continuum subtraction is performed,× and the resulting line maps and integrated Pa α line fluxes are presented. A statistical analysis indicates that the average Pa α surface brightness in the central regions is highest in early-type (Sa-Sb) spirals. Subject headings: infrared:galaxies—infrared:ISM:lines and bands—galaxies:nuclei— galaxies:starburst—galaxies:statistics 1Affiliated with the Astrophysics Division, Space Science Department, European Space Agency 1 1. Introduction with the NIC3 F190N filter. The velocity range was chosen such that the Pa α line falls well inside the NICMOS is a second generation HST instrument, high transmission region of the respective filter, with installed during the HST servicing mission in Febru- only minor corrections ( 5%) needed to account for ary 1997. -
Outflow Versus Infall in Spiral Galaxies: Metal Absorption in the Halo of Ngc 891
OUTFLOW VERSUS INFALL IN SPIRAL GALAXIES: METAL ABSORPTION IN THE HALO OF NGC 891 The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Bregman, Joel N., Eric D. Miller, Patrick Seitzer, C. R. Cowley, and Matthew J. Miller. “OUTFLOW VERSUS INFALL IN SPIRAL GALAXIES: METAL ABSORPTION IN THE HALO OF NGC 891.” The Astrophysical Journal 766, no. 1 (March 7, 2013): 57. © 2013 The American Astronomical Society As Published http://dx.doi.org/10.1088/0004-637x/766/1/57 Publisher IOP Publishing Version Final published version Citable link http://hdl.handle.net/1721.1/94577 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astrophysical Journal, 766:57 (6pp), 2013 March 20 doi:10.1088/0004-637X/766/1/57 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. OUTFLOW VERSUS INFALL IN SPIRAL GALAXIES: METAL ABSORPTION IN THE HALO OF NGC 891 Joel N. Bregman1, Eric D. Miller2, Patrick Seitzer1,C.R.Cowley1, and Matthew J. Miller1 1 Department of Astronomy, University of Michigan, Ann Arbor, MI 48105, USA; [email protected] 2 Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA Received 2010 July 8; accepted 2013 January 7; published 2013 March 7 ABSTRACT Gas accreting onto a galaxy will be of low metallicity while halo gas due to a galactic fountain will be of near-solar metallicity. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Nuclear Properties of Nearby Spiral Galaxies from Hubble Space Telescope NICMOS Imaging and STIS Spectroscopy
Nuclear Properties of Nearby Spiral Galaxies from Hubble Space Telescope NICMOS imaging and STIS Spectroscopy.1 M. A. Hughes1, D. Axon11, J. Atkinson1, A. Alonso-Herrero2, C. Scarlata7, A. Marconi4, D. Batcheldor1, J. Binney6, A. Capetti5, C. M. Carollo7, L. Dressel3, J. Gerssen12, D. Macchetto3, W. Maciejewski4,10, M. Merrifield8, M. Ruiz1, W. Sparks3, M. Stiavelli3, Z. Tsvetanov9, ABSTRACT We investigate the central regions of 23 spiral galaxies using archival NICMOS imag- ing and STIS spectroscopy. The sample is taken from our program to determine the masses of central massive black holes (MBH) in 54 nearby spiral galaxies. Stars are likely to contribute significantly to any dynamical central mass concentration that we find in our MBH program and this paper is part of a series to investigate the nuclear properties of these galaxies. We use the Nuker law to fit surface brightness profiles, derived from the NICMOS images, to look for nuclear star clusters and find possible extended sources in 3 of the 23 galaxies studied (13 per cent). The fact that this fraction is lower than that inferred from optical Hubble Space Telescope studies is probably due to the greater spatial resolution of those studies. Using R-H and J-H colors and equiv- alent widths of Hα emission (from the STIS spectra) we investigate the nature of the stellar population with evolutionary models. Under the assumption of hot stars ionizing the gas, as opposed to a weak AGN, we find that there are young stellar populations (∼10–20 Myr) however these data do not allow us to determine what percentage of the 1Centre for Astrophysical Research, STRI, University of Hertfordshire, Hatfield, Hertfordshire, AL10 9AB, UK. -
Warm Ionized Medium.Pdf
IVie. UJc^u-^ -Xo^^hl^ M^ckovx^ (covWVJ i- (o l<-) y SL-ock, io-^.lc^Vv^v A^-3 5"2?>, 2-Z3 \truvi A ^ TV, ^"4? (^ ^& ^^^ . Xr v^^ cU^c^^ £ cuTU. T- •*_. <r**VZ lfcS<B3 _\.fcS*i° ? \ i>\ \ ^-QA vv£W >jirv 3 <QD o ck: o-A- \^ cL^tv^*> c ^O - i. ; &*&>} ;w*.o _- _e^ - \r*e ^ 6t^M^^^ ^ tm t* ^*si**o uor^c- 2.\<^c c^.-vw^— <r*,> « O.C25 V O.ovb <a o— ^^-, LOvH E. K^ ', -»i -^ K^Qj&ff**'^ V"W. £^Q V^ J»S^\ C/V^ C,awvXv^^ >jl!laa.<A To oq ~TW ReM a^<£A* GLg>^ rto^wu^ C*o*«0 ; c^^rf^ , tV*\V^ ^"T^V^- ^^ z/zrr^ Lo^ (VV°'Z' AA o = e.fnA>«-1 » eV% i-'l »t- <T^ <r"° CJL. s"L^ »Wa4^ ^ A-»^f\JCL p-^OOe^ ©aj<oa(2o c^L 4-cJ5t^^ CI) <^©a^ • #0 ^T^a_j f^TU ^e^^cy <-(\eJU.s ~ ^^1 ;^.*pU£w^__ S~\ - 2 ^ /u^ lA erf T^ T^ *occ^fL HlT^^ T- <Lx^«^ 3Xj^ WoT A<S^7 "^v*-*-^^*&b ^vx.cUv-c^CA^ ^TW*n ^^ %^^>^e^s^N.^ . VW^ C^^o) Jh*~** C«^j ,vc Qa-^j—^JT '. 'p'^a-^^ovAJL VQ©£-4>>~-Cc . oJ vTtv &-a^ < 1i s 2T- t^H ^%U= o.ofe cm!3 = Woo K <u^ } ^^r A- uio^ -^ojt-v. Haj&la, OKiK CotOH , TUcis is* puAcT^i To occcaw. (—- TUa_ HeVc^-GV^VU^ CO\f\ at the UR des an distri- ^dium, 5 basic those atures solar *ate is stend- •out I , e.g., )f ion- log Ih. -
Galaxies: Outstanding Problems and Instrumental Prospects for the Coming Decade (A Review)* T (Cosmology/History of Astronomy/Quasars/Space) JEREMIAH P
Proc. Natl. Acad. Sci. USA Vol. 74, No. 5, pp. 1767-1774, May 1977 Astronomy Galaxies: Outstanding problems and instrumental prospects for the coming decade (A Review)* t (cosmology/history of astronomy/quasars/space) JEREMIAH P. OSTRIKER Princeton University Observatory, Peyton Hall, Princeton, New Jersey 08540 Contributed by Jeremiah P. Ostriker, February 3, 1977 ABSTRACT After a review of the discovery of external It is more than a little astonishing that in the early part of this galaxies and the early classification of these enormous aggre- century it was the prevailing scientific view that man lived in gates of stars into visually recognizable types, a new classifi- a universe centered about himself; by 1920 the sun's newly cation scheme is suggested based on a measurable physical quantity, the luminosity of the spheroidal component. It is ar- discovered, slightly off-center position was still controversial. gued that the new one-parameter scheme may correlate well The discovery was, ironically, due to Shapley. both with existing descriptive labels and with underlying A little background to this debate may be useful. The Island physical reality. Universe hypothesis was not new, having been proposed 170 Two particular problems in extragalactic research are isolated years previously by the English astronomer, Thomas Wright as currently most fundamental. (i) A significant fraction of the (2), and developed with remarkably prescience by Emmanuel energy emitted by active galaxies (approximately 1% of all galaxies) is emitted by very small central regions largely in parts Kant, who wrote (see refs. 10 and 23 in ref. 3) in 1755 (in a of the spectrum (microwave, infrared, ultraviolet and x-ray translation from Edwin Hubble). -
Corrugated Velocity Patterns in the Spiral Galaxies: NGC 278, NGC 1058, NGC 2500 & UGC 3574
Mem. S.A.It. Suppl. Vol. 25, 86 Memorie della c SAIt 2013 Supplementi Corrugated velocity patterns in the spiral galaxies: NGC 278, NGC 1058, NGC 2500 & UGC 3574 M. C. Sanchez´ Gil1, E. J. Alfaro2, and E. Perez´ 2 1 Universidad de Cadiz,´ Facultad de Ciencias Poligono Rio San Pedro 11510 - Puerto Real, Spain, e-mail: [email protected] 2 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), E18008, Granada, Spain Abstract. In this work we address the study of the detection in Hα of a radial corruga- tion in the vertical velocity field in a sample of four nearly face-on, spiral galaxies. The geometry of the problem is a main criterion in the selection of the sample as well as of the azimuthal angle of the slits. These spatial corrugations must be equally associated with wavy vertical motions in the galactic plane with a strong large-scale consistency. Evidence of these kinematic waves were first detected in the analysis of the rotation curves of spiral galaxies (eg Vaucoleurs & de Vaucaleurs 1963, Pismis 1965), but it was not until 2001 that Alfaro et al. analyzed in more detail the velocity corrugations in NGC 5427 and a possi- ble physical mechanism for their origin. The aim of this study is to analyze the corrugated velocity pattern in terms of the star formation processes. We describe the geometry of the problem and establish its fundamental relationships. Key words. Techniques: spectroscopic–Galaxies: kinematics and dynamics - spiral - struc- ture 1. Introduction & Delgado 1992) and both in the azimuthal direction along different spiral arms (Spicker The disks of spiral galaxies are highly struc- & Feitzinger 1986), as in the radial, in differ- tured. -
Extraplanar HII Regions in the Edge-On Spiral Galaxies NGC 3628 and NGC 4522? Y
A&A 605, A5 (2017) DOI: 10.1051/0004-6361/201730589 Astronomy & c ESO 2017 Astrophysics Extraplanar HII regions in the edge-on spiral galaxies NGC 3628 and NGC 4522? Y. Stein1, D. J. Bomans1; 2, A. M. N. Ferguson3, and R.-J. Dettmar1; 2 1 Astronomisches Institut (AIRUB), Ruhr-Universität Bochum, Universitätsstrasse 150, 44801 Bochum, Germany e-mail: [email protected] 2 Research Department: Plasmas with Complex Interactions, Ruhr-Universität Bochum, Universitätsstrasse 150, 44801 Bochum, Germany 3 Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK Received 9 February 2017 / Accepted 30 May 2017 ABSTRACT Context. Gas infall and outflow are critical for determining the star formation rate and chemical evolution of galaxies but direct measurements of gas flows are difficult to make. Young massive stars and Hii regions in the halos of galaxies are potential tracers for accretion and/or outflows of gas. Aims. Gas phase abundances of three Hii regions in the lower halos of the edge-on galaxies NGC 3628 and NGC 4522 are determined by analyzing optical long-slit spectra. The observed regions have projected distances to the midplane of their host from 1.4 to 3 kpc. Methods. With the measured flux densities of the optical nebular emission lines, we derived the oxygen abundance 12 + log(O/H) for the three extraplanar Hii regions. The analysis was based on one theoretical and two empirical strong-line calibration methods. Results. The resulting oxygen abundances of the extraplanar Hii regions are comparable to the disk Hii regions in one case and are a little lower in the other case. -
Lopsided Spiral Galaxies: Evidence for Gas Accretion
A&A 438, 507–520 (2005) Astronomy DOI: 10.1051/0004-6361:20052631 & c ESO 2005 Astrophysics Lopsided spiral galaxies: evidence for gas accretion F. Bournaud1, F. Combes1,C.J.Jog2, and I. Puerari3 1 Observatoire de Paris, LERMA, 61 Av. de l’Observatoire, 75014 Paris, France e-mail: [email protected] 2 Department of Physics, Indian Institute of Science, Bangalore 560012, India 3 Instituto Nacional de Astrofísica, Optica y Electrónica, Calle Luis Enrique Erro 1, 72840 Tonantzintla, Puebla, Mexico Received 3 January 2005 / Accepted 15 March 2005 Abstract. We quantify the degree of lopsidedness for a sample of 149 galaxies observed in the near-infrared from the OSUBGS sample, and try to explain the physical origin of the observed disk lopsidedness. We confirm previous studies, but for a larger sample, that a large fraction of galaxies have significant lopsidedness in their stellar disks, measured as the Fourier amplitude of the m = 1 component normalised to the average or m = 0 component in the surface density. Late-type galaxies are found to be more lopsided, while the presence of m = 2 spiral arms and bars is correlated with disk lopsidedness. We also show that the m = 1 amplitude is uncorrelated with the presence of companions. Numerical simulations were carried out to study the generation of m = 1viadifferent processes: galaxy tidal encounters, galaxy mergers, and external gas accretion with subsequent star formation. These simulations show that galaxy interactions and mergers can trigger strong lopsidedness, but do not explain several independent statistical properties of observed galaxies. To explain all the observational results, it is required that a large fraction of lopsidedness results from cosmological accretion of gas on galactic disks, which can create strongly lopsided disks when this accretion is asymmetrical enough.