J/MNRAS/452/549 ALHAMBRA survey galaxy clusters and groups (Ascaso+, 2015)
Galaxy clusters and groups in the ALHAMBRA survey.
Ascaso B., Benitez N., Fernandez-Soto A., Arnalte-Mur P., Lopez-Sanjuan C.,
Molino A., Schoenell W., Jimenez-Teja Y., Merson A.I., Huertas-Company M.,
Diaz-Garcia L.A., Martinez V.J., Cenarro A.J., Dupke R., Marquez I.,
Masegosa J., Nieves-Seoane L., Povic M., Varela J., Viironen K.,
Aguerri J.A.L., Del Olmo A., Moles M., Perea J., Alfaro E.,
Aparicio-Villegas T., Broadhurst T., Cabrera-Cano J., Castander F.J.,
Cepa J., Cervino M., Gonzalez Delgado R.M., Cristobal-Hornillos D.,
Hurtado-Gil L., Husillos C., Infante L., Prada F., Quintana J.M.
<Mon. Not. R. Astron. Soc., 452, 549-565 (2015)>
=2015MNRAS.452..549A 2015MNRAS.452..549A (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Redshifts
Keywords: catalogues - galaxies: clusters: general - galaxies: evolution -
cosmology: observations - large-scale structure of Universe -
X-rays: galaxies: clusters
Abstract:
We present a catalogue of 348 galaxy clusters and groups with
0.2<z<1.2 selected in the 2.78deg2 Advanced Large, Homogeneous Area
Medium Band Redshift Astronomical (ALHAMBRA) survey. The high
precision of our photometric redshifts, close to 1 percent, and the
wide spread of the seven ALHAMBRA pointings ensure that this catalogue
has better mass sensitivity and is less affected by cosmic variance
than comparable samples. The detection has been carried out with the
Bayesian Cluster Finder, whose performance has been checked in
ALHAMBRA-like light-cone mock catalogues. Great care has been taken to
ensure that the observable properties of the mocks photometry
accurately correspond to those of real catalogues. From our
simulations, we expect to detect galaxy clusters and groups with both
70 percent completeness and purity down to dark matter halo masses of
Mh∼3x1013M☉ for z<0.85. Cluster redshifts are expected to be
recovered with ∼0.6 percent precision for z<1. We also expect to
measure cluster masses with sigmaMh|M*CL_∼0.25-0.35dex precision
down to ∼3x1013M☉, masses which are 50 percent smaller than
those reached by similar work. We have compared these detections with
previous optical, spectroscopic and X-rays work, finding an excellent
agreement with the rates reported from the simulations. We have also
explored the overall properties of these detections such as the
presence of a colour-magnitude relation, the evolution of the
photometric blue fraction and the clustering of these sources in the
different ALHAMBRA fields. Despite the small numbers, we observe
tentative evidence that, for a fixed stellar mass, the environment is
playing a crucial role at lower redshifts (z<0.5).
Description:
The ALHAMBRA (http://alhambrasurvey.com) (Moles et al.,
2008AJ....136.1325M 2008AJ....136.1325M) survey is a 20 narrow-band optical and three
broad-band NIR (JHK) photometric survey imaged with the wide-field
cameras LAICA and OMEGA-2000, respectively, at the Calar Alto
Observatory (Spain).
In this work, we have used the BCF (Ascaso et al., 2012, Highlights of
Spanish Astrophysics VII. Guirado J. C., Lara L. M., Quilis V., Gorgas
J., editors. 2013. p. 115. Proceedings of the X Scientific Meeting of
the Spanish Astronomical Society (SEA), July 9-13, 2012. Valencia), a
technique developed to detect galaxy clusters and groups in any
optical/infrared image data set. This method is based on a
modification of the Matched Filter Technique (Postman et al., 2002,
Cat. J/ApJ/579/93) including photometric redshifts and the presence of
Bayesian priors.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 125 352 Clusters and groups detected in the ALHAMBRA
survey with Level 1 and 2 of completeness and
purity
table3.dat 125 174 Clusters and groups detected in the ALHAMBRA
survey with Level 3 of completeness and purity
not included in Table 2
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See also:
J/ApJ/579/93 : KPNO/Deeprange distant cluster survey (Postman+, 2002)
J/AJ/139/1242 : ALHAMBRA photometric system (Villegas+, 2010)
J/MNRAS/435/3444 : ALHAMBRA survey morphological catalogue (Povic+, 2013)
Byte-by-byte Description of file: table2.dat table3.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq Sequential number
5- 13 A9 --- Field Field name
15- 32 A18 --- Name ALHAMBRA name (ALHHHMM.SS+DDMM.SS) (1)
34- 35 I2 h RAh Right ascension (J2000)
37- 38 I2 min RAm Right ascension (J2000)
40- 44 F5.2 s RAs Right ascension (J2000)
46 A1 --- DE- Declination sign (J2000)
47- 48 I2 deg DEd Declination (J2000)
50- 51 I2 arcmin DEm Declination (J2000)
53- 57 F5.2 arcsec DEs Declination (J2000)
59- 68 F10.6 deg RAdeg Right ascension (J2000)
70- 76 F7.4 deg DEdeg Declination (J2000)
78- 81 F4.2 --- zprob Probable photometric redshift
83- 88 F6.4 --- zest Estimated photometric redshift
90- 95 F6.4 --- e_zest rms uncertainty on zest
97-102 F6.2 --- LambdaCL LambdaCL parameter (2)
104-112 E9.4 Msun MstarCL Cluster mass
114-122 E9.4 Msun Mhalo Dark matter halo mass
124-125 A2 --- Level Level (L1, L2 or L3)
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Note (1): Caution: Original names where mis-printed in the following cases:
ALHHHMM.S+DDMM.SS stands for ALHHHMM.0S+DDMM.SS
ALHHHMM.SS+DDMM.S stands for ALHHHMM.SS+DDMM.0S
The names have been corrected in the tables,
as example :
ALH0226.60+0107.2 02 26 59.98 +01 07 01.56 corrected into ALH0226.60+0107.02
ALH0230.5+0035.51 02 30 04.68 +00 35 51.36 corrected into ALH0230.05+0035.51
Note (2): the LambdaCL parameter is the sum of the luminosity of the galaxies
(in the F814W band) statistically belonging to the cluster divided by the
characteristic luminosity L* .
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 14-Jan-2016