The Evolution of Structure and Feedback with Arcus
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Lemmings. I. the Emerlin Legacy Survey of Nearby Galaxies. 1.5-Ghz Parsec-Scale Radio Structures and Cores
MNRAS 000,1{44 (2018) Preprint 8 February 2018 Compiled using MNRAS LATEX style file v3.0 LeMMINGs. I. The eMERLIN legacy survey of nearby galaxies. 1.5-GHz parsec-scale radio structures and cores R. D. Baldi1?, D. R. A. Williams1, I. M. McHardy1, R. J. Beswick2, M. K. Argo2;3, B. T. Dullo4, J. H. Knapen5;6, E. Brinks7, T. W. B. Muxlow2, S. Aalto8, A. Alberdi9, G. J. Bendo2;10, S. Corbel11;12, R. Evans13, D. M. Fenech14, D. A. Green15, H.-R. Kl¨ockner16, E. K¨ording17, P. Kharb18, T. J. Maccarone19, I. Mart´ı-Vidal8, C. G. Mundell20, F. Panessa21, A. B. Peck22, M. A. P´erez-Torres9, D. J. Saikia18, P. Saikia17;23, F. Shankar1, R. E. Spencer2, I. R. Stevens24, P. Uttley25 and J. Westcott7 1 School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK 2 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK 3 Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK 4 Departamento de Astrofisica y Ciencias de la Atmosfera, Universidad Complutense de Madrid, E-28040 Madrid, Spain 5 Instituto de Astrofisica de Canarias, Via Lactea S/N, E-38205, La Laguna, Tenerife, Spain 6 Departamento de Astrofisica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain 7 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK 8 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 43992 Onsala, Sweden 9 Instituto de Astrofisica de Andaluc´ıa(IAA, CSIC); Glorieta de la Astronom´ıa s/n, 18008-Granada, Spain 10 ALMA Regional Centre Node, UK 11 Laboratoire AIM (CEA/IRFU - CNRS/INSU - Universit´eParis Diderot), CEA DSM/IRFU/SAp, F-91191 Gif-sur-Yvette, France 12 Station de Radioastronomie de Nan¸cay, Observatoire de Paris, PSL Research University, CNRS, Univ. -
GHASP: an Halpha Kinematic Survey of Spiral and Irregular Galaxies - IV
GHASP: an Halpha kinematic survey of spiral and irregular galaxies - IV. 44 new velocity fields. Extension, shape and asymmetry of Halpha rotation curves P. Amram, C. Balkowski, J. Boulesteix, J.L. Gach, O. Garrido, M. Marcelin To cite this version: P. Amram, C. Balkowski, J. Boulesteix, J.L. Gach, O. Garrido, et al.. GHASP: an Halpha kinematic survey of spiral and irregular galaxies - IV. 44 new velocity fields. Extension, shape and asymmetry of Halpha rotation curves. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2005, 362, pp.127. 10.1111/j.1365-2966.2005.09274.x. hal-00017198 HAL Id: hal-00017198 https://hal.archives-ouvertes.fr/hal-00017198 Submitted on 13 Dec 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Mon. Not. R. Astron. Soc. 362, 127–166 (2005) doi:10.1111/j.1365-2966.2005.09274.x GHASP: an Hα kinematic survey of spiral and irregular galaxies – IV. 44 new velocity fields. Extension, shape and asymmetry of Hα rotation curves , O. Garrido,1 2 M. Marcelin,2 P. Amram,2 C. Balkowski,1 J. -
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. -
X-Ray Spectral Variability of Seyfert 2 Galaxies⋆
A&A 579, A90 (2015) Astronomy DOI: 10.1051/0004-6361/201526127 & c ESO 2015 Astrophysics X-ray spectral variability of Seyfert 2 galaxies L. Hernández-García1,J.Masegosa1, O. González-Martín2, and I. Márquez1 1 Instituto de Astrofísica de Andalucía, CSIC, Glorieta de la Astronomía, s/n, 18008 Granada, Spain e-mail: [email protected] 2 Centro de radioastronomía y Astrofísica (CRyA-UNAM), 3-72 (Xangari), 8701 Morelia, Mexico Received 18 March 2015 / Accepted 2 May 2015 ABSTRACT Context. Variability across the electromagnetic spectrum is a property of active galactic nuclei (AGN) that can help constrain the physical properties of these galaxies. Nonetheless, the way in which the changes happen and whether they occur in the same way in every AGN are still open questions. Aims. This is the third in a series of papers with the aim of studying the X-ray variability of different families of AGN. The main purpose of this work is to investigate the variability pattern(s) in a sample of optically selected Seyfert 2 galaxies. Methods. We use the 26 Seyfert 2s in the Véron-Cetty and Véron catalog with data available from Chandra and/or XMM-Newton public archives at different epochs, with timescales ranging from a few hours to years. All the spectra of the same source were simultaneously fitted, and we let different parameters vary in the model. Whenever possible, short-term variations from the analysis of the light curves and/or long-term UV flux variations were studied. We divided the sample into Compton-thick and Compton-thin candidates to account for the degree of obscuration. -
Metallicity at the Explosion Sites of Interacting Transients⋆⋆⋆
A&A 580, A131 (2015) Astronomy DOI: 10.1051/0004-6361/201525989 & c ESO 2015 Astrophysics Metallicity at the explosion sites of interacting transients F. Taddia1, J. Sollerman1, C. Fremling1, A. Pastorello2, G. Leloudas3,4, C. Fransson1, A. Nyholm1, M. D. Stritzinger5, M. Ergon1,R.Roy1, and K. Migotto1 1 The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm, Sweden e-mail: [email protected] 2 INAF–Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 3 Department of Particle Physics & Astrophysics, Weizmann Institute of Science, Rehovot 76100, Israel 4 Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, 2100 Copenhagen, Denmark 5 Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, 8000 Aarhus C, Denmark Received 28 February 2015 / Accepted 28 May 2015 ABSTRACT Context. Some circumstellar-interacting (CSI) supernovae (SNe) are produced by the explosions of massive stars that have lost mass shortly before the SN explosion. There is evidence that the precursors of some SNe IIn were luminous blue variable (LBV) stars. For a small number of CSI SNe, outbursts have been observed before the SN explosion. Eruptive events of massive stars are named SN impostors (SN IMs) and whether they herald a forthcoming SN or not is still unclear. The large variety of observational properties of CSI SNe suggests the existence of other progenitors, such as red supergiant (RSG) stars with superwinds. Furthermore, the role of metallicity in the mass loss of CSI SN progenitors is still largely unexplored. Aims. Our goal is to gain insight into the nature of the progenitor stars of CSI SNe by studying their environments, in particular the metallicity at their locations. -
3.2 Polarization Studies of Spiral Galaxies 62
Durham E-Theses Optical polarimetry studies of Seyfert galaxies Felton, Michelle Ann How to cite: Felton, Michelle Ann (1999) Optical polarimetry studies of Seyfert galaxies, Durham theses, Durham University. Available at Durham E-Theses Online: http://etheses.dur.ac.uk/4573/ Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in Durham E-Theses • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full Durham E-Theses policy for further details. Academic Support Oce, Durham University, University Oce, Old Elvet, Durham DH1 3HP e-mail: [email protected] Tel: +44 0191 334 6107 http://etheses.dur.ac.uk Optical polarimetry studies of Seyfert galaxies Michelle Ann Felton B.Sc. (Theoretical Physics) M.Sc. (Radio Astronomy) The copyright of this thesis rests witli die author. No quotation from it should be published without the written consent of the author and information derived from it should be acknowledged. A thesis submitted to the University of Durham for the degree of Doctor of Philosophy 1 4 NOV 2000 Department of Physics University of Durham Durham September 1999 Abstract Optical imaging polarimetry has been performed on seven nearby Seyfert galaxies, three with face-on and four with edge-on host galaxies of various morphological classifications. -
Arxiv:1502.07024V2
Draft version September 2, 2018 A Preprint typeset using LTEX style emulateapj v. 12/16/11 HIDING IN PLAIN SIGHT: AN ABUNDANCE OF COMPACT MASSIVE SPHEROIDS IN THE LOCAL UNIVERSE Alister W. Graham1, Bililign T. Dullo, Giulia A.D. Savorgnan Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC, 3122, Australia. Draft version September 2, 2018 ABSTRACT It has been widely remarked that compact, massive, elliptical-like galaxies are abundant at high redshifts but exceedingly rare in the Universe today, implying significant evolution such that their sizes at z ∼ 2 ± 0.6 have increased by factors of 3 to 6 to become today’s massive elliptical galaxies. These claims have been based on studies which measured the half-light radii of galaxies as though they are all single component systems. Here we identify 21 spheroidal stellar systems within 90 Mpc 11 11 that have half-light, major-axis radii Re . 2 kpc, stellar masses 0.7 × 10 < M∗/M⊙ < 1.4 × 10 , and S´ersic indices typically around a value of n = 2 to 3. This abundance of compact, massive spheroids in our own backyard — with a number density of 6.9 × 10−6 Mpc−3 (or 3.5×10−5 Mpc−3 per unit dex in stellar mass) — and with the same physical properties as the high-redshift galaxies, had been over-looked because they are encased in stellar disks which usually result in galaxy sizes notably larger than 2 kpc. Moreover, this number density is a lower limit because it has not come from a volume-limited sample. -
The Westerbork HI Survey of Spiral and Irregular Galaxies
A&A 442, 137–157 (2005) Astronomy DOI: 10.1051/0004-6361:20053172 & c ESO 2005 Astrophysics The Westerbork HI survey of spiral and irregular galaxies III. HI observations of early-type disk galaxies E. Noordermeer1,J.M.vanderHulst1, R. Sancisi1,2,R.A.Swaters3,andT.S.vanAlbada1 1 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands e-mail: [email protected] 2 INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy 3 Department of Astronomy, University of Maryland, College Park, MD 20742-2421, USA Received 1 April 2005 / Accepted 29 June 2005 ABSTRACT We present H observations of 68 early-type disk galaxies from the WHISP survey. They have morphological types between S0 and Sab and absolute B-band magnitudes between –14 and –22. These galaxies form the massive, high surface-brightness extreme of the disk galaxy population, few of which have been imaged in H before. The H properties of the galaxies in our sample span a large range; the average values of MHI/LB and DHI/D25 are comparable to the ones found in later-type spirals, but the dispersions around the mean are larger. No significant differences are found between the S0/S0aandtheSa/Sab galaxies. Our early-type disk galaxies follow the same H mass-diameter relation as later-type spiral galaxies, but their effective H surface densities are slightly lower than those found in later-type systems. In some galaxies, distinct rings of H emission coincide with regions of enhanced star formation, even though the average gas densities are far below the threshold of star formation derived by Kennicutt (1989, ApJ, 344, 685). -
B, V, R, I, H and K Images of 86 Face-On Spiral Galaxies
B, V , R, I, H and K images of 86 face-on spiral galaxies Roelof S. de Jong(1,2) (1) University of Durham, Dept. of Physics, South Road, Durham DH1 3LE, United Kingdom [[email protected]] (2) Kapteyn Astronomical Institute, P.O.box 800, 9700 AV Groningen, The Netherlands November 12, 2018 Abstract FITS images in the B, V , R, I, H and K passbands are presented of a sample of 86 face-on spiral galaxies. The galaxies were selected from the UGC to have a diameter of at least 2′ and a minor over major axis ratio larger than 0.625. The selected galaxies o have an absolute Galactic latitude |b| > 25 , to minimize the effect of Galactic extinction and foreground stars. Nearly all BVRI data were obtained with the 1m Jacobus Kapteyn Telescope at La Palma and the H and K data were obtained at the 3.8m UK Infra-Red Telescope at Hawaii. The field of view of the telescope/camera combinations were often smaller than the observed galaxies, therefore driftscanning and mosaicing techniques were employed to image at least along the major axis of the galaxies. Most images were obtained during photometric nights and calibrated using standard stars. A small fraction of the images was calibrated from literature aperture photometry. The azimuthally averaged radial luminosity profiles derived from these galaxy images (see de Jong and van der Kruit 1994, Paper I) are also made available in machine readable format, as are the results of the bulge/disk decompositions described in de Jong (1996a, Paper II). -
Hot Gaseous Halos Around Galaxies
HOT GASEOUS HALOS AROUND GALAXIES by Michael E. Anderson A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy (Astronomy and Astrophysics) in The University of Michigan 2013 Doctoral Committee: Professor Joel N. Bregman, Chair Associate Professor Eric F. Bell Professor August Evrard Associate Professor Oleg Y. Gnedin Assistant Professor Christopher J. Miller Associate Professor Jon M. Miller Associate Professor Mateusz Ruszkowski Michael E. Anderson Copyright c 2013 All Rights Reserved To my parents, with love ii ACKNOWLEDGMENTS It is a pleasure to acknowledge the many people and institutions upon whom I have relied during my graduate studies at Michigan. It has been a wonderful experience working with and learning from my advisor, Joel Bregman. I greatly admire his combination of uncannily prescient leaps of big-picture intuition paired with scrupulous attention to details, and to the extent I have learned to think more like a scientist during my PhD program, Joel deserves the credit for this. He has also been unwaveringly supportive of me throughout this process. I really appreciate his willingness to take me on as an unexpected PhD student, his availability, assistance, and forbearance with technical issues large and small, and his insights into the wider culture of academia. The rest of my thesis committee – Eric Bell, Gus Evrard, Oleg Gnedin, Chris Miller, Jon Miller, and Mateusz Ruszkowski – have also helped me in a number of ways. Joel, Eric, and Oleg have been incredibly supportive of Astrocoffee, and I have learned an enormous amount from their lively debates. Jon went out of his way to welcome me to the program and to guide me through the thicket of relevant depart- mental and Rackham requirements. -
Study of LINER Sources with Broad Hα Emission
A&A 530, A149 (2011) Astronomy DOI: 10.1051/0004-6361/201116806 & c ESO 2011 Astrophysics Study of LINER sources with broad Hα emission. X-ray properties and comparison to luminous AGN and X-ray binaries G. Younes1, D. Porquet1,B.Sabra2, and J. N. Reeves3 1 Observatoire Astronomique de Strasbourg, Université de Strasbourg, CNRS, UMR7550, 11 Rue de l’Université, 67000 Strasbourg, France e-mail: [email protected] 2 Department of Physics & Astronomy, Notre Dame University-Louaize, PO Box 72, Zouk Mikael, Lebanon 3 Astrophysics Group, School of Physical & Geographical Sciences, Keele University, Keele, Staffordshire ST5 5BG, UK Received 1 March 2011 / Accepted 19 April 2011 ABSTRACT Context. An important number of multiwavelength studies of low ionization nuclear emission-line regions (LINERs) were dedicated to investigate the excitation mechanism responsible for the detected emission lines. Radiative emission from accretion into a super massive black hole (SMBH) is now believed to be, in an increasing number of LINERs, the source of excitation. However, the accretion mode is not yet firmly understood, and could be explained in either a thin accretion disk or a radiatively inefficient accretion flow (RIAF). Aims. Our purpose is to study the X-ray properties of LINER sources with definite detection of a broad Hα emission line in their optical spectra, LINER 1s from Ho et al. sample. These objects preferentially harbor a low luminosity active nucleus at the center and show small or no intrinsic absorption (≤1022 cm−1). We compare their X-ray properties to both X-ray binaries and luminous AGN. Methods. -
DSO List V2 Current
7000 DSO List (sorted by constellation - magnitude) 7000 DSO List (sorted by constellation - magnitude) - from SAC 7.7 database NAME OTHER TYPE CON MAG S.B. SIZE RA DEC U2K Class ns bs SAC NOTES M 31 NGC 224 Galaxy AND 3.4 13.5 189' 00 42.7 +41 16 60 Sb Andromeda Galaxy;Local Group;nearest spiral NGC 7686 OCL 251 Opn CL AND 5.6 - 15' 23 30.1 +49 08 88 IV 1 p 20 6.2 H VIII 69;12* mags 8...13 NGC 752 OCL 363 Opn CL AND 5.7 - 50' 01 57.7 +37 40 92 III 1 m 60 9 H VII 32;Best in RFT or binocs;Ir scattered cl 70* m 8... M 32 NGC 221 Galaxy AND 8.1 12.4 8.5' 00 42.7 +40 52 60 E2 Companion to M31; Member of Local Group M 110 NGC 205 Galaxy AND 8.1 14 19.5' 00 40.4 +41 41 60 SA0 M31 Companion;UGC 426; Member Local Group NGC 272 OCL 312 Opn CL AND 8.5 - 00 51.4 +35 49 90 IV 1 p 8 9 NGC 7662 PK 106-17.1 Pln Neb AND 8.6 5.6 17'' 23 25.9 +42 32 88 4(3) 14 Blue Snowball Nebula;H IV 18;Barnard-cent * variable? NGC 956 OCL 377 Opn CL AND 8.9 - 8' 02 32.5 +44 36 62 IV 1 p 30 9 NGC 891 UGC 1831 Galaxy AND 9.9 13.6 13.1' 02 22.6 +42 21 62 Sb NGC 1023 group;Lord Rosse drawing shows dark lane NGC 404 UGC 718 Galaxy AND 10.3 12.8 4.3' 01 09.4 +35 43 91 E0 Mirach's ghost H II 224;UGC 718;Beta AND sf 6' IC 239 UGC 2080 Galaxy AND 11.1 14.2 4.6' 02 36.5 +38 58 93 SBa In NGC 1023 group;vsBN in smooth bar;low surface br NGC 812 UGC 1598 Galaxy AND 11.2 12.8 3' 02 06.9 +44 34 62 Sbc Peculiar NGC 7640 UGC 12554 Galaxy AND 11.3 14.5 10' 23 22.1 +40 51 88 SBbc H II 600;nearly edge on spiral MCG +08-01-016 Galaxy AND 12 - 1.0' 23 59.2 +46 53 59 Face On MCG +08-01-018