Extensive near-infrared (<i>H</i>-band) photometry in Coma

Andreon, S.; Pelló, R.; Davoust, E.; Domínguez, Raimundo; Poulain, P.

doi:10.1051/aas:2000112

Cited by 33 publications

(63 citation statements)

References 14 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A rough estimate of how much the LF is skewed by adopting magnitudes that are know to miss flux (and whole galaxies) can be guessed by comparing two determinations of the LF of AC 118: the first one is computed by using a 3 arcsec aperture (Andreon 2002) and agrees with both determinations of the local LF, while the second one adopts our surrogate of "total" mag (Andreon 2001): the LF is shallower by 0.3 in α and fainter by 0.9 mag in M * (but be aware that errors on best fit parameters are strongly coupled and therefore other pairs of values give almost equivalent descriptions of the difference).…”

Section: Discussionmentioning

confidence: 99%

“…However, this dependence cannot be definitively ruled out because the Pahre sample is not complete and the dependence is expected via the correlation between absolute magnitude and surface brightness of galaxies (faint galaxies tend to be of low surface brightness, Andreon & Cuillandre 2002).…”

Section: Mass Isophotal Magnitudes and The Kochanek Et Al Lfmentioning

confidence: 99%

“…For AC 118 galaxies (at z = 0.3) our (Andreon 2002) 3 arcsec aperture magnitude (16 Kpc for galaxies at the AC 118 redshift) is not a surrogate for "total magnitude": we checked that a lot of flux is lost by comparing 3 arcsec aperture magnitude to both our surrogate of "total" magnitude (figure not shown) and to total mags of Pahre galaxies (redshifted at the cluster redshift, figure not shown). Therefore, the LF computed Fig.…”

Section: Aperture Magnitude and Lfs Based On Themmentioning

confidence: 99%

See 2 more Smart Citations

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

Andreon

2002

A&A

Self Cite

View full text Add to dashboard Cite

Abstract. By using high-resolution and deep Ks band observations of early-type galaxies of the nearby Universe and of a cluster at z = 0.3 we show that the two luminosity functions (LFs) of the local universe derived from 2MASS data miss a fair fraction of the flux of the galaxies (more than 20 to 30%) and a whole population of galaxies of central brightness fainter than the isophote used for detection, but bright enough to be included in the published LFs. In particular, the fraction of lost flux increases as the galaxy surface brightness become fainter. Therefore, the so far derived LF slopes and characteristic luminosity as well as luminosity density are underestimated. Other published near-infrared LFs miss flux in general, including the LF of the distant field computed in a 3 arcsec aperture.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Mass Isophotal Magnitudes and The Kochanek Et Al Lfmentioning

confidence: 99%

Section: Aperture Magnitude and Lfs Based On Themmentioning

confidence: 99%

See 1 more Smart Citation

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

Andreon

2002

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…In Fig. 4 the composite LF is compared to the local cluster galaxies K band LF (corrected by 1.3 mag for passive evolution as derived below) as measured in Coma by De Propris et al (1998) and Andreon & Pelló (2000), and in samples of nearby clusters by Balogh et al (2001) and Lin et al (2004). All the local and field LFs have been arbitrarily rescaled.…”

Section: Composite Luminosity Functionmentioning

confidence: 99%

The near-infrared luminosity function of cluster galaxies beyond redshift one

Strazzullo

Rosati

Stanford

et al. 2006

A&A

View full text Add to dashboard Cite

Aims. We determined the K s band luminosity function (LF), and inferred the corresponding stellar mass function, of cluster galaxies at redshift z 1.2, using near-infrared images of three X-ray luminous clusters at z = 1.11, 1.24, 1.27. Methods. The composite LF was derived down to M * + 4, by means of statistical background subtraction, and is well described by a Schechter function with K * s = 20.5 +0.4−1 and α = −1.0 +0.2 −0.3 . Using available X-ray mass profiles we determined the M/L ratios of these three clusters, which tend to be lower than those measured in the local universe. Finally, from the K s band composite LF we derived the stellar mass function of cluster galaxies. Results. With these data, no significant difference can be seen between the cluster galaxies LF and the LF of field galaxies at similar redshift. We also found no significant evolution out to z 1.2 in the bright ( 2. Conclusions. The results obtained in this work support and extend previous findings that most of the stars in bright galaxies were formed at high redshift, and that K s -bright (M > 10 11 M ) galaxies were already in place at z 1.2, at least in the central regions of X-ray luminous clusters. Together with recent results on the field galaxy stellar mass function, this implies that most of the stellar mass is already assembled in massive galaxies by z 1, both in low and high density environments.

show abstract

“…After the catalogue of galaxies in the Coma cluster (Godwin et al 1983), several studies on this cluster have been published in different wavelength windows (e.g. Donas et al 1991;Biviano et al 1995;Lobo et al 1997;Andreon 1999;Andreon & Pelló 2000). Considering the optical R-band alone, there is little agreement in the literature on the faint-end slope of the LF.…”

Section: Introductionmentioning

confidence: 99%

Ther'-band luminosity function of Abell 1367: A comparison with Coma

Iglésias-Páramo¹,

Boselli²,

Gavazzi³

et al. 2002

A&A

View full text Add to dashboard Cite

Abstract. We made a large (approximately 1• × 1 • ) r -band imaging survey of the central regions of the two nearby clusters of galaxies, Abell 1367 and Coma. The data, presented as a catalog, are used to construct the r -band luminosity function (LF) of galaxies in these two clusters, by subtracting the Yasuda et al. (2001) galaxy counts from our cluster counts. Our Coma luminosity function is consistent with previous determinations, i.e. providing a faint end slope α = −1.47 +0.08−0.09 , significantly steeper than the one we find for Abell 1367 (α = −1.07 +0.20 −0.16 ). The counts in Abell 1367 show a relative minimum at r ≈ 19, followed by a steep increase faintward. The difference between the two clusters appears significant, given the consistency of the experimental conditions in the two clusters. Whereas for Coma we find a significant increase of the slope of the LF outwards, no such effect is found for Abell 1367.

show abstract

Extensive near-infrared (H-band) photometry in Coma

Cited by 33 publications

References 14 publications

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

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

The near-infrared luminosity function of cluster galaxies beyond redshift one

Ther'-band luminosity function of Abell 1367: A comparison with Coma

Contact Info

Product

Resources

About