Dim galaxies and outer halos of galaxies missed by 2MASS? The near–infrared luminosity function and density

Andreon, S.

doi:10.1051/0004-6361:20011636

Cited by 46 publications

(64 citation statements)

References 21 publications

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“…To correct for the missed flux (and hence mass) coming from the galaxy outer regions (e.g., Blanton et al 2001;Andreon 2002a,b) and the intracluster light we increased the measured flux of all radial bins by 15% (Blanton et al 2001;Andreon 2002aAndreon ,b, 2010Andreon , 2012Bahcall & Kulier 2014). 3. Characteristic mass, faint-end slope, and surface density stellar mass profile…”

Section: Samples and Datamentioning

confidence: 99%

Relative distribution of dark matter and stellar mass in three massive galaxy clusters

Andreon

2015

A&A

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This work observationally addresses the relative distribution of total and optically luminous matter in galaxy clusters by computing the radial profile of the stellar-to-total mass ratio. We adopt state-of-the-art accurate lensing masses free from assumptions about the mass radial profile and we use extremely deep multicolor wide-field optical images to distinguish star formation from stellar mass, to properly calculate the mass in galaxies of low mass, those outside the red sequence, and to allow a contribution from galaxies of low mass that is clustercentric dependent. We pay special attention to issues and contributions that are usually underrated, yet are major sources of uncertainty, and we present an approach that allows us to account for all of them. Here we present the results for three very massive clusters at z ∼ 0.45, MACSJ1206.2-0847, MACSJ0329.6-0211, and RXJ1347.5-1145. We find that stellar mass and total matter are closely distributed on scales from about 150 kpc to 2.5 Mpc: the stellar-to-total mass ratio is radially constant. We find that the characteristic mass stays constant across clustercentric radii and clusters, but that the less-massive end of the galaxy mass function is dependent on the environment.

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Section: Samples and Datamentioning

confidence: 99%

Relative distribution of dark matter and stellar mass in three massive galaxy clusters

Andreon

2015

A&A

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“…Andreon 2002Andreon , 2006Andreon , 2008Andreon , 2010Andreon et al 2006Andreon et al , 2008Meyers et al 2012). We accounted for the background (galaxies in the cluster line-of-sight), estimated in adjacent lines-of-sight.…”

Section: The Data and Analysismentioning

confidence: 99%

Observational evidence that massive cluster galaxies were forming stars atz~ 2.5 and did not grow in mass at later times

Andreon

2013

A&A

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Using Spitzer 3.6 micron data we derived the luminosity function and the mass function of galaxies in five z > 1.4 clusters selected to have a firm intracluster medium detection. The five clusters differ in richness (ISCS J1438.1+3414 and XMMXCS J2215.9-1738 are twice as rich as ISCS J1432.4+3250, IDCS J1426.5+3508, and JKCS 041) and morphological appareance. At the median redshift z = 1.5, from the 150 member galaxies of the five clusters, we derived a characteristic magnitude of 16.92 ± 0.13 in the [3.6] band and a characteristic mass of lg M * = 11.30 ± 0.05 M . We find that the characteristic luminosity and mass does not evolve between z = 1 and 1.4 < z < 1.8, directly ruling out ongoing mass assembly between these epochs because massive galaxies are already present up to z = 1.8. Lower-redshift build-up epochs have already been ruled out by previous works, leaving only z > 1.8 as a possible epoch for the mass build up. However, the observed values of m * at very high redshift are too bright for galaxies without any star formation immediately preceding the observed redshift and therefore imply a star formation episode not earlier than z f = 2.5. For the first time, mass/luminosity functions are able to robustly distinguish tiny differences between formation redshifts and to set upper limits to the epoch of the last star-formation episode.

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“…In our previous work, we studied the Coma cluster using a complete spectroscopic sample for its inner 25 (De Propris et al 1998). Skelton et al (2009) We have elected not to use 2MASS (Skrutskie et al 2006) photometry, except for purposes of calibration, as this is known to miss a considerable fraction of the flux for bright galaxies and to be incomplete for fainter ones (Andreon 2002;Kirby et al 2008). We confirm this by comparison with our photometry: on average, 2MASS magnitudes (we use the homogeneous 14 aperture for reference, which should be large enough to include all the flux) are systematically ∼ 0.3 mag.…”

Section: Introductionmentioning

confidence: 99%

TheK-band luminosity functions of cluster galaxies

Propris¹

2016

Mon. Not. R. Astron. Soc.

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We derive the galaxy luminosity function in the K s band for galaxies in 24 clusters to provide a local reference for higher redshift studies and to analyse how and if the luminosity function varies according to environment and cluster properties. We use new, deep K band imaging and match the photometry to available redshift information and to optical photometry from the SDSS or the UKST/POSS: > 80% of the galaxies to K ∼ 14.5 have measured redshifts. We derive composite luminosity functions, for the entire sample and for cluster subsamples . We consider the luminosity functions for red sequence and blue cloud galaxies. The full composite luminosity function has K * = 12.79 ± 0.14 (M K = −24.81) and α = −1.41 ± 0.10. We find that K * is largely unaffected by the environment but that the slope α increases towards lower mass clusters and clusters with Bautz-Morgan type < II. The red sequence luminosity function seems to be approximately universal (within errors) in all environments: it has parameters K * = 13.16 ± 0.15 (M K = −24.44) and α = −1.00 ± 0.12 (for all galaxies). Blue galaxies do not show a good fit to a Schechter function, but the best values for its parameters are K * = 13.51 ± 0.41 (M K = −24.09) and α = −1.60 ± 0.29: we do not have enough statistics to consider environmental variations for these galaxies. We find some evidence that K * in clusters is brighter than in the field and α is steeper, but note this comparison is based (for the field) on 2MASS photometry, while our data are considerably deeper.

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Dim galaxies and outer halos of galaxies missed by 2MASS? The near–infrared luminosity function and density

Cited by 46 publications

References 21 publications

Relative distribution of dark matter and stellar mass in three massive galaxy clusters

Relative distribution of dark matter and stellar mass in three massive galaxy clusters

Observational evidence that massive cluster galaxies were forming stars atz~ 2.5 and did not grow in mass at later times

TheK-band luminosity functions of cluster galaxies

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