J/PASP/122/261 Herschel Reference Survey Sample (Boselli+, 2010)
The Herschel Reference Survey.
Boselli A., Eales S., Cortese L., Bendo G., Chanial P., Buat V., Davies J.,
Auld R., Rigby E., Baes M., Barlow M., Bock J., Bradford M.,
Castro-Rodriguez N., Charlot S., Clements D., Cormier D., Dwek E.,
Elbaz D., Galametz M., Galliano F., Gear W., Glenn J., Gomez H.,
Griffin M., Hony S., Isaak K., Levenson L., Lu N., Madden S.,
O'Halloran B., Okamura K., Oliver S., Page M., Panuzzo P., Papageorgiou A.,
Parkin T., Perez-Fournon I., Pohlen M., Rangwala N., Roussel H., Rykala A.,
Sacchi N., Sauvage M., Schulz B., Schirm M., Smith M.W.L., Spinoglio L.,
Stevens J., Symeonidis M., Vaccari M., Vigroux L., Wilson C., Wozniak H.,
Wright G., Zeilinger W.
<Publ. Astron. Soc. Pac. 122, 261 (2010)>
=2010PASP..122..261B 2010PASP..122..261B
ADC_Keywords: Galaxy catalogs ; Radial velocities ; Photometry, infrared
Abstract:
The Herschel Reference Survey is a Herschel guaranteed time key
project and will be a benchmark study of dust in the nearby universe.
The survey will complement a number of other Herschel key projects
including large cosmological surveys that trace dust in the distant
universe. We will use Herschel to produce images of a
statistically-complete sample of 323 galaxies at 250, 350, and 500um.
The sample is volume-limited, containing sources with distances
between 15 and 25Mpc and flux limits in the K band to minimize the
selection effects associated with dust and with young high-mass stars
and to introduce a selection in stellar mass. The sample spans the
whole range of morphological types (ellipticals to late-type spirals)
and environments (from the field to the center of the Virgo Cluster)
and as such will be useful for other purposes than our own. We plan to
use the survey to investigate (i) the dust content of galaxies as a
function of Hubble type, stellar mass, and environment; (ii) the
connection between the dust content and composition and the other
phases of the interstellar medium; and (iii) the origin and evolution
of dust in galaxies. In this article, we describe the goals of the
survey, the details of the sample and some of the auxiliary observing
programs that we have started to collect complementary data. We also
use the available multifrequency data to carry out an analysis of the
statistical properties of the sample.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 142 323 The Herschel Reference Sample
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- HRS [1/323] Herschel Reference Sample number
5- 10 I6 --- CGCG ?=- CGCG (Cat. VII/190) number
12- 15 I4 --- VCC ?=- VCC (Cat. J/AJ/90/1681) number
17- 20 I4 --- UGC ?=- UGC (Cat. VII/26) number
22- 25 I4 --- NGC ?=- NGC (Cat. VII/118) number
26 A1 --- m_NGC [A] Multiplicity index on NGC
28- 31 I4 --- IC ?=- IC (Cat. VII/118) number
33- 34 I2 h RAh Right ascension (J2000)
36- 37 I2 min RAm Right ascension (J2000)
39- 43 F5.2 s RAs Right ascension (J2000)
45 A1 --- DE- Declination sign (J2000)
46- 47 I2 deg DEd Declination (J2000)
49- 50 I2 arcmin DEm Declination (J2000)
52- 55 F4.1 arcsec DEs Declination (J2000)
57- 76 A20 --- MType Morphological type
78- 82 F5.2 mag Ksmag 2MASS total Ks magnitude
84- 88 F5.2 arcmin D25 Optical isophotal diameter (25mag/arcsec2)
90- 93 I4 km/s HRV Heliocentric radial velocity, from HI data
when available, otherwise from NED
95-113 A19 --- Mem Cluster or cloud membership (1)
115-116 A2 --- Gr Pair/group membership (2)
118-121 F4.2 mag AB Galactic extinction (Schlegel et al.,
1998ApJ...500..525S 1998ApJ...500..525S)
123-142 A20 --- OName Other name(s)
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Note (1): From Gavazzi et al. (1999MNRAS.304..595G 1999MNRAS.304..595G) for Virgo, and Tully
(1988, Cat. VII/118) or Nolthenius (1993ApJS...85....1N 1993ApJS...85....1N) whenever
available, or from our own estimate otherwise.
Note (2): Karachentsev et al. (1972, Cat. VII/77) or from NED whenever
available, or from our own estimate elsewhere. Pair/group membership
has been assigned according to the following criteria:
CP = close pairs are those with a nearby companion at a distance less
than 50kpc and a difference in redshift <600km/s, as in
Gavazzi et al. (1999A&AS..136..227G 1999A&AS..136..227G),
P = pairs up to 150kpc.
3 = galaxy belongs to a triplet
4 = galaxy belongs to a quadruplet
5 = galaxy belongs to a quintuplet
Groups outside Virgo and its immediate surroundings have been
determined by counting the number of bright galaxies within 25'
(which, at a median distance of 20Mpc, corresponds to 150kpc) and
600km/s. Pairs in the Virgo region are only those catalogued by
Karachentsev et al. (1972, Cat. VII/77).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 04-Apr-2010