DOCSLIB.ORG

Astronomy Astrophysics

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Astronomy Astrophysics A&A 463, 493–502 (2007) Astronomy DOI: 10.1051/0004-6361:20066109 & c ESO 2007 Astrophysics The age structure of globular cluster systems in early-type galaxies and its dependence on host galaxy properties M. Hempel1,2, M. Kissler-Patig3,T.H.Puzia4, and M. Hilker3,5 1 Michigan State University, Department of Physics and Astronomy, 48824 East Lansing, Michigan, USA 2 University of Florida, Department of Astronomy, 211 Bryant Space Science Center, Gainesville 32611, FL, USA e-mail: [email protected] 3 European Southern Observatory, Karl-Schwarzschild Str. 2, 85748 Garching, Germany e-mail: [email protected] 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: [email protected] 5 Argelander Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany e-mail: [email protected] Received 25 July 2006 / Accepted 13 October 2006 ABSTRACT Aims. We present the results of an optical – near-infrared photometric survey of globular cluster systems in early-type galaxies. Our project aims to study correlations between the age structure of the globular cluster systems and environmental as well as structural parameters of their host galaxies. Methods. To derive the age structure in globular cluster systems we use combined optical and near-infrared photometry. This com- bination facilitates the detection of young globular cluster sub-populations if their age differs significantly from the old (∼13 Gyr) population, i.e. if their age is ∼<7 Gyr. We investigate globular cluster systems in galaxies located in the central regions of galaxy clusters (NGC 1399, M 87, NGC 4478), galaxies which are members of (sub-) groups (NGC 4365, NGC 5846) and isolated galaxies (NGC 3115 and NGC 7192). Further, we look for correlations between globular cluster system properties and structural parame- ters of the galaxies (velocity dispersion σ, color ((V − K), (B − V)), and luminosity MV ). For a quantitative analysis we define the “Methuselah” parameter, Mth – based on the fraction of young and old metal-rich globular clusters weighted by age, characterizing the age structure of a globular cluster system. Results. We find that, within our galaxy sample, group galaxies appear to host an intermediate-age globular cluster population, whereas the globular cluster systems in cluster galaxies and in rather isolated galaxies are dominated by an old globular cluster popu- lation. A weak correlation of Mth with the Hβ index of the integrated light of the host galaxies is the only trend found with respect to internal galaxy parameters. Key words. galaxies: star clusters – galaxies: formation – galaxies: evolution – galaxies: fundamental parameters 1. Tracing the star formation episodes in early-type population, consisting of an old stellar population and being sim- galaxies ilar in their basic features (e.g. see Bender & Renzini 2005, and contributions therein). However, detailed spectroscopic investi- The formation, evolution and star formation history of galaxies gations of the integrated light of nearby galaxies revealed a va- remains one of the most active fields in observational astronomy. riety of structural features (e.g. Gorgas et al. 1990; Bender & Based on various photometric and spectroscopic studies of early- Surma 1992; Bender et al. 1992; de Zeeuw et al. 2002, the type galaxies (and their globular cluster systems) our picture of SAURON survey and references therein), that were neither ex- these galaxies as an old, uniform, and rather predictable class of pected nor visible in photometric studies. Counter- or co-rotating objects has changed significantly. cores as well as massive dust shells turned out to be rather com- Various features of early-type galaxies are well explained mon amongst early-type galaxies and are clearly a sign of a more by the commonly accepted formation scenarios, whereas oth- active evolution of these objects. An open question is whether ers are in complete contradiction to it (e.g. Pahre 1999a). The these morphological signatures of a turbulent past also imply a fundamental plane (e.g. Djorgovski & Davis 1987; Dressler significant perturbation of the star formation history of the host et al. 1987), for instance, proved to be compatible over a galaxy. In order to answer this question, sub-populations of dif- long look-back time with an early major star-formation epoch. ferent ages must be detected in the host galaxy, which proved to Overall, early-type galaxies appear to form a very homogeneous be very difficult by using the integrated light only. In contrast, identifying these sub-populations in the globular cluster systems Based on observations at the Very Large Telescope of the European appears to be a more promising route. Southern Observatory, Chile (Program 63.N-0287, 64.N-0102). By representing single stellar populations (SSPs) and as a Founded by merging of the Sternwarte, Radioastronomisches sign of the major star formation episodes, globular clusters are Institut and Institut für Astrophysik und Extraterrestrische Forschung ideal probes of the evolutionary history of the parent galaxy. der Universität Bonn. In order to assemble statistically relevant galaxy samples, Article published by EDP Sciences and available at http://www.aanda.org or http://dx.doi.org/10.1051/0004-6361:20066109 494 M. Hempel et al.: Early-type galaxies: compilation Table 1. Relevant properties of our sample galaxies. The information was taken from: (1) de Vaucouleurs et al. (1991); (2) Tully & Fisher (1988); (3) NED Data base and references therein; (4) Pahre (1999b); (5) Beuing et al. (2002). Property NGC 1399 NGC 1426 NGC 3115 NGC 4478 NGC 4365 M 87 NGC 5846 NGC 7192 Location Fornax (cD) Fornax (c) Leo (g) Virgo Virgo (c) Virgo (cD) Virgo-Libra (g) ρ[Mpc−3] (2) 1.59 0.66 0.08 3.92 2.93 4.17 0.84 0.28 m − M (1) 31.14 31.13 29.12 31.13 31.13 31.13 32.27 32.76 Type(1)E1E4S0E2E3E+0-1,pec E0-1 SA0 BT,0 (1) 10.44 12.26 9.74 12.21 10.49 9.49 10.91 12.19 (B − V) (2,3) 1.26 0.89 1.04 0.60 1.05 0.86 1.07 0.97 (V − K)0 (3) 3.28 2.71 3.02 3.09 2.92 2.82 3.12 2.64 MV (2,3) –21.55 –19.74 –20.22 –19.78 –21.57 –22.50 –22.23 –21.52 σ [km s−1] (2) 308 155 264 143 261 333 252 184 Hβ[Å] (5) 1.19 – 1.85 1.84 1.73 1.07 2.02 1.51 (∆Hβ)[Å] (5) (±0.16) – (±0.11) (±0.06) (±0.12) (±0.25) (±0.09) (±0.09) D25(4) 3.3 2.2 6.1 1.9 6.2 9.2 4.9 1.7 Peculiarities radio jet – – – KDC radio dust KDC – – – – – X-ray X-ray - Abbreviations: KDC- kinematically distinct core; c- galaxy cluster; g- galaxy group; cD- central cluster galaxy. representing a specific set of galaxy parameters (e.g. environ- formation and evolution models and to compare them with the ment, luminosity, ...), efficient photometric studies are used. mean ages derived for intermediate and high redshift galaxies. Once the existence of age sub-populations within the globular The method constructs, from color−color diagrams, cumu- cluster system has been established photometrically, more ac- lative age distributions based on a comparison with population curate ages for sub-sets of globular clusters can be determined synthesis isochrones. Cumulative age distributions are computed using spectroscopy (e.g. Puzia et al. 2005). for the observed data, as well as for many Monte-Carlo simula- The combination of optical and near-infrared photometry tions assuming two sub-populations of varying age and relative of globular clusters (e.g. Goudfrooij et al. 2001; Kissler-Patig fraction. The observed and simulated distributions are compared, et al. 2002; Puzia et al. 2002; Hempel & Kissler-Patig 2004) and the best model is assumed for the observed galaxy. Some de- has been introduced in order to reduce the degeneracy of age tails are given below. and metallicity effects and to allow the resolution of globular cluster age sub-populations. With the availability of infrared im- 2.2. The observational basis: color–color diagrams agers on 8−10 m class telescopes, such as ISAAC (Infrared Spectrometer And Array Camera) at the Very Large Telescope The observational basis of the method are the optical-infrared (VLT) or space based instruments (e.g. NICMOS on board color−color diagrams. They are shown in Fig. 1 for our eight Hubble Space Telescope or IRAC on board the Spitzer Space sample galaxies. From these, it becomes clear that a direct pho- Telescope) we are now able to complement, for a large galaxy tometric determination of the absolute ages of individual globu- sample, the vast number of optical data sets with infrared data. lar clusters is not possible. Here we present results of our ongoing study on early-type However, the density distribution of objects in a diagram can galaxies, which includes 8 galaxies, varying in parameters such be compared to the location of simple stellar population (SSP) as environment (represented by the Tully density parameter ρ), models. In our analysis, we used models by Bruzual & Charlot luminosity, velocity dispersion, and color. Basic information on (2003); Vazdekis (1999); Maraston (2005) to probe the model the galaxy sample is given in Table 1. dependence of our results. A visual inspection of Fig. 1 allows us to identify differences between the various galaxies: most sys- tems have the majority of their clusters scattered around the old- 2. The age structure of a globular cluster system est (here 13 Gyr) isochrone, while a few systems show a large fraction of clusters below that isochrone, i.e.
Load more

Recommended publications
  • WALLABY Pre-Pilot Survey: Two Dark Clouds in the Vicinity of NGC 1395
    University of Texas Rio Grande Valley ScholarWorks @ UTRGV Physics and Astronomy Faculty Publications and Presentations College of Sciences 2021 WALLABY pre-pilot survey: Two dark clouds in the vicinity of NGC 1395 O. I. Wong University of Western Australia A. R. H. Stevens B. Q. For University of Western Australia Tobias Westmeier M. Dixon See next page for additional authors Follow this and additional works at: https://scholarworks.utrgv.edu/pa_fac Part of the Astrophysics and Astronomy Commons, and the Physics Commons Recommended Citation O I Wong, A R H Stevens, B-Q For, T Westmeier, M Dixon, S-H Oh, G I G Józsa, T N Reynolds, K Lee-Waddell, J Román, L Verdes-Montenegro, H M Courtois, D Pomarède, C Murugeshan, M T Whiting, K Bekki, F Bigiel, A Bosma, B Catinella, H Dénes, A Elagali, B W Holwerda, P Kamphuis, V A Kilborn, D Kleiner, B S Koribalski, F Lelli, J P Madrid, K B W McQuinn, A Popping, J Rhee, S Roychowdhury, T C Scott, C Sengupta, K Spekkens, L Staveley-Smith, B P Wakker, WALLABY pre-pilot survey: Two dark clouds in the vicinity of NGC 1395, Monthly Notices of the Royal Astronomical Society, 2021;, stab2262, https://doi.org/10.1093/ mnras/stab2262 This Article is brought to you for free and open access by the College of Sciences at ScholarWorks @ UTRGV. It has been accepted for inclusion in Physics and Astronomy Faculty Publications and Presentations by an authorized administrator of ScholarWorks @ UTRGV. For more information, please contact [email protected], [email protected].
    [Show full text]
  • X-Ray Luminosities for a Magnitude-Limited Sample of Early-Type Galaxies from the ROSAT All-Sky Survey
    Mon. Not. R. Astron. Soc. 302, 209±221 (1999) X-ray luminosities for a magnitude-limited sample of early-type galaxies from the ROSAT All-Sky Survey J. Beuing,1* S. DoÈbereiner,2 H. BoÈhringer2 and R. Bender1 1UniversitaÈts-Sternwarte MuÈnchen, Scheinerstrasse 1, D-81679 MuÈnchen, Germany 2Max-Planck-Institut fuÈr Extraterrestrische Physik, D-85740 Garching bei MuÈnchen, Germany Accepted 1998 August 3. Received 1998 June 1; in original form 1997 December 30 Downloaded from https://academic.oup.com/mnras/article/302/2/209/968033 by guest on 30 September 2021 ABSTRACT For a magnitude-limited optical sample (BT # 13:5 mag) of early-type galaxies, we have derived X-ray luminosities from the ROSATAll-Sky Survey. The results are 101 detections and 192 useful upper limits in the range from 1036 to 1044 erg s1. For most of the galaxies no X-ray data have been available until now. On the basis of this sample with its full sky coverage, we ®nd no galaxy with an unusually low ¯ux from discrete emitters. Below log LB < 9:2L( the X-ray emission is compatible with being entirely due to discrete sources. Above log LB < 11:2L( no galaxy with only discrete emission is found. We further con®rm earlier ®ndings that Lx is strongly correlated with LB. Over the entire data range the slope is found to be 2:23 60:12. We also ®nd a luminosity dependence of this correlation. Below 1 log Lx 40:5 erg s it is consistent with a slope of 1, as expected from discrete emission.
    [Show full text]
  • X-Ray Constraints on the Local Supermassive Black Hole
    Draft version November 11, 2018 A Preprint typeset using LTEX style emulateapj v. 5/2/11 X-RAY CONSTRAINTS ON THE LOCAL SUPERMASSIVE BLACK HOLE OCCUPATION FRACTION Brendan P. Miller,1,2 Elena Gallo,1 Jenny E. Greene,3 Brandon C. Kelly,4 Tommaso Treu,4 Jong-Hak Woo5, & Vivienne Baldassare1 Draft version November 11, 2018 ABSTRACT Distinct seed formation mechanisms are imprinted upon the fraction of dwarf galaxies currently containing a central supermassive black hole. Seeding by Pop III remnants is expected to produce a higher occupation fraction than is generated with direct gas collapse precursors. Chandra observations of nearby early-type galaxies can directly detect even low-level supermassive black hole activity, and the active fraction immediately provides a firm lower limit to the occupation fraction. Here, we use the volume-limited AMUSE surveys of ∼200 optically-selected early-type galaxies to characterize simultaneously, for the first time, the occupation fraction and the scaling of LX with Mstar, accounting for intrinsic scatter, measurement uncertainties, and X-ray limits. For early-type galaxies with Mstar < 10 10 M⊙, we obtain a lower limit to the occupation fraction of >20% (at 95% confidence), but full occupation cannot be excluded. The preferred dependence of log LX upon log Mstar has a slope of ∼0.7–0.8, consistent with the “downsizing” trend previously identified from the AMUSE dataset, and a uniform Eddington efficiency is disfavored at ∼2σ. We provide guidelines for the future precision with which these parameters may be refined with larger or more sensitive samples. Subject headings: black hole physics — galaxies: nuclei 1.
    [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]
  • 1985Apj. ..291 ...8M the Astrophysical Journal
    8M .... The Astrophysical Journal, 291:8-31,1985 April 1 © 1985. The American Astronomical Society. All rights reserved. Printed in U.S.A. ..291 1985ApJ. DYNAMICS OF LUMINOUS GALAXIES. II. SURFACE PHOTOMETRY AND VELOCITY DISPERSIONS OF BRIGHTEST CLUSTER MEMBERS Eliot M. Malumuth1 and Robert P. Kirshner1,2 Department of Astronomy, University of Michigan Received 1983 September 9 ; accepted ]984 October 8 ABSTRACT Velocity dispersions for 46 galaxies and CCD surface photometry for 27 galaxies have been obtained using the McGraw-Hill Observatory 1.3 m and the KPNO No. 1 0.9 m telescopes. The results provide a greatly improved set of data for investigating the brightest galaxies in galaxy clusters. We find that the brightest cluster members (BCMs) are substantially brighter than predicted from their velocity dispersions and the Loca4 relation for elliptical galaxies. In the range of velocity dispersion from 193 to 346 km s-1, the BCMs average 1.22 mag brighter than E galaxies. We consider the possibility that this might be a selection effect due to the spread of M at given a, but show that the observed distribution of luminosity excess does not corre- spond to a simple model of selection unless the elliptical galaxy sample suffers a Malmquist bias of 0.4 mag. We note that our data show that the BCMs with the largest excess luminosity have the largest effective radii and the lowest surface brightnesses, as predicted by homologous merger models. One result that is not predict- ed by simple merger models is that the surface brightness profiles of the galaxies which have the largest excess luminosities are the flattest.
    [Show full text]
  • Nearby Early-Type Galaxies with Ionized Gas. II. Line-Strength Indices
    Astronomy & Astrophysics manuscript no. paper April 23, 2017 (DOI: will be inserted by hand later) Nearby early–type galaxies with ionized gas.II. Line-strength indices for 18 additional galaxies⋆ Annibali F.1, Bressan A.1,2, Rampazzo R.2, Zeilinger W.W.3 1 SISSA, via Beirut 4 - 34014 Trieste - Italy 2 INAF - Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, Italy 3Institut f¨ur Astronomie der Universit¨at Wien, T¨urkenschanzstraße 17, A-1180 Wien, Austria Received date; accepted date Abstract. Rampazzo et al. 2005 (hereafter Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum to Paper I enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, namely NGC 3607, NGC 5077 and NGC 5898 have been already presented in the previous set). As in Paper I, we measured 25 line–strength indices, defined by the Lick IDS “standard” system (Trager et al. 1998; Worthey & Ottaviani 1997), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature. Key words. Galaxies: elliptical and lenticular, cD – Galaxies: fundamental parameters – Galaxies: formation – Galaxies: evolution 1. Introduction lution with time (see e.g. Buzzoni et al. 1992; Worthey 1992; Gonz´alez 1993; Buzzoni et al.
    [Show full text]
  • ASEM Newsletter December2015
    ASEM Newsletter December2015 Comet C/2013 US10 Catalina December 1st, 2015 image from Gregg Ruppel December Calendar Social December 3 – 7-9pm Beginner Meeting @ Weldon Springs Interpretive Center, 7295 HWY 94 South, St. Charles, MO 63304 December 12 – Monthly Meeting. 5pm Open House, hors d’oeuvres @ Weldon Springs Interpretive Center, 7295 HWY 94 South, St. Charles, MO 63304. 6pm ham dinner provided by Marv and Barb Stewart followed by monthly meeting at 7pm. Complimentary dishes and desserts are welcome. Carla Kamp is turning over hospitality hosting duties with the January meeting. December 22- 7pm DigitalSIG Astrophoto group meeting Weldon Spring, 7295 Highway 94 South, St. Charles, MO 63304. Note this is the FOURTH Tuesday for just this month. We’ll go back to the 3rd Tuesday in January. December 23- 7PM DIY-ATMSIG Weldon Spring, 7295 Highway 94 South, St. Charles, MO 63304 December 4, 11, 18, 25- 7 pm start times Broemmelsiek Park Public viewing, weather permitting. ASTRONOMICAL DELIGHTS If you’re very careful, on December 7 a very old crescent moon will occult Venus in daylight, late morning. You’ll need to look to the west of the sun-don’t catch the sun in your binoculars- around 11:10 or so for the disappearance on the bright side of the moon. Start your search before 11am so you know where Venus and the moon are. Venus will be occulted for about 90 minutes. There’s a really good lunar libration on December 21 at the north Polar region. Good night to poke around the north polar landscape craters that are not normally discernible.
    [Show full text]
  • A Database of Cepheid Distance Moduli and TRGB, GCLF, PNLF and SBF Data Useful for Distance Determinations
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server A Database of Cepheid Distance Moduli and TRGB, GCLF, PNLF and SBF Data Useful for Distance Determinations Accepted for publication in the Astrophysical Journal Supplement Series Laura Ferrarese1;2 Holland C. Ford3, John Huchra4, Robert C. Kennicutt, Jr.5, Jeremy R. Mould6, Shoko Sakai7 Wendy L. Freedman8, Peter B. Stetson9, Barry F. Madore10,BradK. Gibson11,JohnA.Graham12, Shaun M. Hughes13, Garth D. Illingworth14,DanielD.Kelson12, Lucas Macri4,KimSebo6 & N.A. Silbermann10 ABSTRACT We present a compilation of Cepheid distance moduli and data for four secondary distance indicators that employ stars in the old stellar populations: the planetary nebula luminosity function (PNLF), the globular cluster luminosity function (GCLF), the tip of the red giant branch (TRGB), and the surface brightness fluctuation (SBF) method. The database includes all data published as of July 15, 1999. The main strength of this compilation resides in all data being on a consistent and homogeneous system: all Cepheid distances are derived using the same calibration of the period-luminosity relation, the treatment of errors is consistent for all indicators, measurements which are not considered reliable are excluded. As such, the database is ideal for inter-comparing any of the distance indicators considered, or for deriving a Cepheid calibration to any secondary distance indicator, such as the Tully-Fisher 1Hubble Fellow 2California Institute of Technology,
    [Show full text]
  • Optical Follow-Up of Gravitational-Wave Events During the Second Advanced LIGO/ VIRGO Observing Run with the DLT40 Survey
    The Astrophysical Journal, 875:59 (25pp), 2019 April 10 https://doi.org/10.3847/1538-4357/ab0e06 © 2019. The American Astronomical Society. All rights reserved. Optical Follow-up of Gravitational-wave Events during the Second Advanced LIGO/ VIRGO Observing Run with the DLT40 Survey Sheng Yang1,2,3 , David J. Sand4 , Stefano Valenti1 , Enrico Cappellaro3 , Leonardo Tartaglia4,5 , Samuel Wyatt4, Alessandra Corsi6 , Daniel E. Reichart7 , Joshua Haislip7, and Vladimir Kouprianov7,8 (DLT40 collaboration) 1 Department of Physics, University of California, 1 Shields Avenue, Davis, CA 95616-5270, USA; [email protected] 2 Department of Physics and Astronomy Galileo Galilei, University of Padova, Vicolo dell’Osservatorio, 3, I-35122 Padova, Italy 3 INAF Osservatorio Astronomico di Padova, Vicolo dell Osservatorio 5, I-35122 Padova, Italy 4 Department of Astronomy/Steward Observatory, 933 North Cherry Avenue, Room N204, Tucson, AZ 85721-0065, USA 5 Department of Astronomy and The Oskar Klein Centre, AlbaNova University Center, Stockholm University, SE-106 91 Stockholm, Sweden 6 Physics & Astronomy Department,Texas Tech University, Lubbock, TX 79409, USA 7 Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Chapel Hill, NC 27599, USA 8 Central (Pulkovo) Observatory of Russian Academy of Sciences, 196140 Pulkovskoye Avenue 65/1, Saint Petersburg, Russia Received 2019 January 23; revised 2019 March 5; accepted 2019 March 6; published 2019 April 16 Abstract We describe the gravitational-wave (GW) follow-up strategy and subsequent results of the Distance Less Than 40 Mpc survey (DLT40) during the second science run (O2) of the Laser Interferometer Gravitational-wave Observatory and Virgo collaboration (LVC).
    [Show full text]
  • Dave Mitsky's Monthly Celestial Calendar
    Dave Mitsky’s Monthly Celestial Calendar January 2010 ( between 4:00 and 6:00 hours of right ascension ) One hundred and five binary and multiple stars for January: Omega Aurigae, 5 Aurigae, Struve 644, 14 Aurigae, Struve 698, Struve 718, 26 Aurigae, Struve 764, Struve 796, Struve 811, Theta Aurigae (Auriga); Struve 485, 1 Camelopardalis, Struve 587, Beta Camelopardalis, 11 & 12 Camelopardalis, Struve 638, Struve 677, 29 Camelopardalis, Struve 780 (Camelopardalis); h3628, Struve 560, Struve 570, Struve 571, Struve 576, 55 Eridani, Struve 596, Struve 631, Struve 636, 66 Eridani, Struve 649 (Eridanus); Kappa Leporis, South 473, South 476, h3750, h3752, h3759, Beta Leporis, Alpha Leporis, h3780, Lallande 1, h3788, Gamma Leporis (Lepus); Struve 627, Struve 630, Struve 652, Phi Orionis, Otto Struve 517, Beta Orionis (Rigel), Struve 664, Tau Orionis, Burnham 189, h697, Struve 701, Eta Orionis, h2268, 31 Orionis, 33 Orionis, Delta Orionis (Mintaka), Struve 734, Struve 747, Lambda Orionis, Theta-1 Orionis (the Trapezium), Theta-2 Orionis, Iota Orionis, Struve 750, Struve 754, Sigma Orionis, Zeta Orionis (Alnitak), Struve 790, 52 Orionis, Struve 816, 59 Orionis, 60 Orionis (Orion); Struve 476, Espin 878, Struve 521, Struve 533, 56 Persei, Struve 552, 57 Persei (Perseus); Struve 479, Otto Struve 70, Struve 495, Otto Struve 72, Struve 510, 47 Tauri, Struve 517, Struve 523, Phi Tauri, Burnham 87, Xi Tauri, 62 Tauri, Kappa & 67 Tauri, Struve 548, Otto Struve 84, Struve 562, 88 Tauri, Struve 572, Tau Tauri, Struve 598, Struve 623, Struve 645, Struve
    [Show full text]
  • Southern Arp - Declination
    Southern Arp - Declination A B C D E F G H I J 1 DEC RA AM # Object Name Magn. Size Constellation Uranom. Uranom. Millenium 2 1st Ed. 2nd Ed. 3 -22d06m30s 03h42m49.1s AM 0340-221 NGC 1426 13.1 2.6 x 1.7 Eridanus 312 156 355 Vol I 4 -22d16m04s 10h21m57.4s AM 1019-220 NGC 3233 13.5 1.7 x 0.9 Hydra 324 151 875 Vol 2 5 -22d21m17s 09h17m52.9s AM 0915-220 NGC 2835 11 6.6 x 4.4 Hydra 322 152 879 Vol 2 6 -22d22m03s 14h38m26.7s AM 1435-220 IC 4468 13.8 2.2 x 0.6 Libra 332 148 863 Vol 2 7 -22d33m52s 03h40m56.8s AM 0338-224 NGC 1415 12.8 3.5 x 1.8 Eridanus 312 156 355 Vol I 8 -22d40m03s 01h30m29.1s AM 0128-225 NGC 578 11.4 4.9 x 3.1 Cetus 308 158 362 Vol I 9 -22d49m35s 09h59m29.5s AM 0957-223 NGC 3081 12.9 2.1 x 1.6 Hydra 324 152 877 Vol 2 10 -22d50m18s 06h24m35.9s AM 0622-224 NGC 2223 12.4 3.2 x 2.8 Canis Major 317 154 347 Vol I 11 -22d50m58s 12h06m07.2s AM 1203-223 MCG -04-29-006 13 2.9 x 2.1 Corvus 328 150 870 Vol 2 12 -22d51m28s 13h07m44.9s AM 1305-223 MCG -04-31-035 14.4 3 x 0.5 Hydra 330 149 867 Vol 2 13 -22d52m02s 03h02m37.6s AM 0300-230 NGC 1187 11.7 5.5 x 4.1 Eridanus 311 157 357 Vol I 14 -22d56m48s 05h42m00.6s AM 0539-225 MCG -04-14-011 13.4 2.8 x 0.6 Lepus 316 155 349 Vol I 15 -22d58m25s 08h33m22.8s AM 0831-224 NGC 2613 11.2 7.2 x 1.8 Pyxis 321 153 881 Vol 2 16 -23d01m40s 03h38m29.8s AM 0336-231 NGC 1395 11 5.9 x 4.5 Eridanus 312 156 356 Vol I 17 -23d05m12s 11h03m23.8s AM 1100-224 NGC 3511 11.5 5.8 x 2 Crater 326 151 873 Vol 2 18 -23d09m41s 09h23m30.2s AM 0921-225 NGC 2865 12.6 2.5 x 1.8 Hydra 323 152 878 Vol 2 19 -23d09m51s 11h53m57.1s
    [Show full text]