J/MNRAS/452/549     ALHAMBRA survey galaxy clusters and groups   (Ascaso+, 2015)
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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    (SIMBAD/NED BibCode)
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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 2.78deg^2^ 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
    M_h_~3x10^13^M_{sun}_ 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 sigma_Mh_|M*CL_~0.25-0.35dex precision
    down to ~3x10^13^M_{sun}_, 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) 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

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(End)                                      Patricia Vannier [CDS]    14-Jan-2016