J/A+A/626/A14 XMMXCSJ2215.9-1738 galaxies reduced datacubes (Maier+, 2019)
Cluster induced quenching of galaxies in the massive cluster XMMXCSJ2215.9-1738
at z∼1.5 traced by enhanced metallicities inside half R200.
Maier C., Hayashi M., Ziegler B.L., Kodama T.
<Astron. Astrophys. 626, A14 (2019)>
=2019A&A...626A..14M 2019A&A...626A..14M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, spectra
Keywords: galaxies: evolution - galaxies: clusters: general -
galaxies: star formation - galaxies: abundances
Abstract:
Cluster environments at z<0.5 were found to increase the gas
metallicities of galaxies which enter inner regions of the clusters
where the density of the intracluster medium is high enough to remove
their hot halo gas by ram-pressure stripping effects and to stop the
inflow of pristine gas. To extend these studies to z>1, the most
massive clusters known at these redshifts are the sites where these
environmental effects should be more pronounced and more easily
observed with present day telescopes. We explore the massive cluster
XMMXCSJ2215.9-1738 at z∼1.5 with KMOS spectroscopy of Halpha and [NII]
covering a region that corresponds to about one virial radius. Using
published spectroscopic redshifts of 108 galaxies in and around the
cluster we computed the location of galaxies in the projected
velocity-versus-position phase-space to separate our cluster sample
into a virialized region of objects accreted longer ago (roughly
inside half R200) and a region of infalling galaxies. We measured
oxygen abundances for ten cluster galaxies with detected [NII] lines
in the individual galaxy spectra and compared the mass-metallicity
relation of the galaxies inside half R200 with the infalling galaxies
and a field sample at similar redshifts. We find that the oxygen
abundances of individual z∼1.5 star-forming cluster galaxies inside
half R200 are comparable, at the respective stellar mass, to the
higher local SDSS metallicity values. We compare our measurements with
a field galaxy sample from the KMOS3D survey at similar redshifts. We
find that the [NII]/Hα line ratios inside half R200 are higher
by 0.2dex and that the resultant metallicities of the galaxies in the
inner part of the cluster are higher by about 0.1dex, at a given mass,
than the metallicities of infalling galaxies and of field galaxies at
z∼1.5. The enhanced metallicities of cluster galaxies at z∼1.5 inside
0.5 R200 indicate that the density of the intracluster medium in this
massive cluster becomes high enough toward the cluster center such
that the ram pressure exceeds the restoring pressure of the hot gas
reservoir of cluster galaxies. This can remove the gas reservoir and
initiate quenching; although the galaxies continue to form stars,
albeit at slightly lower rates, using the available cold gas in the
disk which is not stripped.
Description:
Here are the reduced data cube fits files of the main sample of
cluster galaxies with spectra presented in Figure 1 of the paper.
KMOS has 24 arms of 14x14-spaxels. Each spaxel has 0.2"x0.2", which
gives a global field of view of 2.8"x2.8" for each arm.
Observations were carried out in the H band, which has a typical
spectral resolution of R∼4000. The total on-source exposure time in
the H band was 2.75h.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 153 6 List of fits datacubes
fits/* . 6 Individual datacubes
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
11- 19 F9.5 deg DEdeg Declination of center (J2000)
21- 22 I2 --- Nx Number of pixels along X-axis
24- 25 I2 --- Ny Number of pixels along Y-axis
27- 30 I4 --- Nz Number of slices
32- 36 F5.3 um blambda [1.425] Lower value of wavelength interval
38- 44 F7.5 um Blambda [1.86678] Upper value of wavelength interval
46- 56 F11.9 um dlambda Resolution
58- 67 A10 "date" Obs.date Observation date (YYYY-MM-DD)
69- 72 I4 Kibyte size Size of FITS file
74-105 A32 --- Title Title of the FITS file
107-153 A47 --- FileName Name of FITS file, in subdirectory fits
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Acknowledgements:
Christian Maier, christian.maier(at)univie.ac.at,
Department of Astrophysics, Vienna, Austria
(End) C. Maier [Dept. Astrophys., Vienna, Austria], P. Vannier [CDS] 03-May-2019