J/A+A/407/791 ACO 370, 2218 and 2390 fluxes at 7 and 15um (Metcalfe+, 2003)
An ISOCAM survey through gravitationally lensing galaxy clusters.
I. Source lists and source counts for A370, A2218 and A2390.
Metcalfe L., Kneib J.-P., McBreen B., Altieri B., Biviano A., Delaney M.,
Elbaz D., Kessler M.F., Leech K., Okumura K., Ott S., Perez-Martinez R.,
Sanchez-Fernandez C., Schulz B.
<Astron. Astrophys. 407, 791 (2003)>
=2003A&A...407..791M 2003A&A...407..791M
ADC_Keywords: Clusters, galaxy ; Infrared sources
Mission_Name: ISO
Keywords: surveys - galaxies: clusters: individual: Abell 370 -
galaxies: clusters: individual: Abell 2218 -
galaxies: clusters: individual: Abell 2390 - gravitational lensing -
infrared: galaxies
Abstract:
ESA's Infrared Space Observatory (ISO) was used to perform a deep
survey with ISOCAM through three massive gravitationally lensing
clusters of galaxies. The total area surveyed depends on source flux,
with nearly seventy square arcminutes covered for the brighter flux
levels in maps centred on the three clusters Abell 370, Abell 2218 and
Abell 2390. We present maps and photometry at 6.7um (hereafter 7um)
and 14.3um (hereafter 15um), showing a total of 145 mid-infrared
sources and the associated source counts.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table4.dat 98 20 15um sources detected in the field of Abell 370
table5.dat 105 46 15um sources detected in the field of Abell 2218
table6.dat 105 28 15um sources detected in the field of Abell 2390
table7.dat 100 11 7um sources detected in the field of Abell 370
table8.dat 101 48 7um sources detected in the field of Abell 2218
table9.dat 103 25 7um sources detected in the field of Abell 2390
--------------------------------------------------------------------------------
See also:
B/iso : ISO Observation Log of validated data (ISO Data Centre, 2001)
VI/101 : ISO Observation Log (ISO Team, 2001)
Byte-by-byte Description of file: table?.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 A3 --- --- [ACO]
5- 12 A8 --- Name Sequential number, NNNN NNa (1)
13 A1 --- f_Name [-+] -: source seen only at 15um
+: source seen only at 7um
15- 19 F5.3 --- Signal Source signal in detector units, at 7 or 15um
21- 25 F5.3 --- e_Signal rms uncertainty on Signal
27- 32 F6.2 --- Sign Significance of the detection
(S/σfloor)
34- 38 F5.3 mJy Flux Flux density, at 7 or 15um
40- 44 F5.3 mJy e_Flux rms uncertainty on Flux
46- 50 D5.3 mJy Flens Intrinsic flux density after correction for
lensing amplification, at 7 or 15um
52- 56 F5.3 mJy e_Flens rms uncertainty on Flens
58- 59 I2 h RAh Right ascension (J2000)
61- 62 I2 min RAm Right ascension (J2000)
64- 67 F4.1 s RAs Right ascension (J2000)
69 A1 --- DE- Declination sign (J2000)
70- 71 I2 deg DEd Declination (J2000)
73- 74 I2 arcmin DEm Declination (J2000)
76- 77 I2 arcsec DEs Declination (J2000)
79- 84 F6.4 --- z ? Spectroscopic redshift (3)
87-103 A17 --- r_z Notes and reference for z (2)
--------------------------------------------------------------------------------
Note (1): In table7.dat:
ISOA221828+ (ACO 2218 28 +) and 45+ ACO 2218 45 + are extended
sources even at ISO resolution. The reduction algorithm is not adapted
to treat extended structure and the transformation of extended
structure has not been characterised. No attempt has been made here to
correct for this in the case of these two cluster sources. For these
sources, the quoted fluxes should be regarded as probable
underestimates, especially in the case of ISOA221828+.
Note (2): Redshift references:
B = Barger et al. (1999AJ....117.2656B 1999AJ....117.2656B)
C = Cowie et al. (2001ApJ...551L...9C 2001ApJ...551L...9C)
Eb = Ebbels et al., 1998MNRAS.295...75E 1998MNRAS.295...75E
I = Ivison et al. (1998MNRAS.298..583I 1998MNRAS.298..583I).
K = Kneib, unpublished.
L1 = LeBorgne et al. (1991A&AS...88..133L 1991A&AS...88..133L)
L2 = LeBorgne et al., 1992A&AS...95...87L 1992A&AS...95...87L
M = Mellier et al. (1988A&A...199...13M 1988A&A...199...13M);
N = NED
P = Pello et al., 1991ApJ...366..405P 1991ApJ...366..405P
S01 = Smail et al. (2001, Cat. J/MNRAS/323/839)
S8 = Soucail et al. (1988A&AS...73..471S 1988A&AS...73..471S);
S9 = Soucail et al. (1999A&A...343L..70S 1999A&A...343L..70S);
Y = Yee et al. (1996, Cat. J/ApJS/102/289)
SED = Spectral fitting
Note (3): the redshift has been assigned to 0 for stars,
or to 0.7 (median redshift of the background population)
for background objects lacking spectroscopic redshift
(the redshift has then no reference assigned).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) James Marcout, Patricia Bauer [CDS] 24-Oct-2003