Calibrating the fundamental plane with SDSS DR8 data

Saulder, Christoph; Mieske, S.; Zeilinger, W. W.; Chilingarian, Igor

doi:10.1051/0004-6361/201321466

Cited by 50 publications

(95 citation statements)

References 68 publications

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“…According to Läsker et al (2013), b19 is a clear outlier of the fundamental plane of Bernardi et al (2003). In contrast to this, we found that b19 is only slightly more than 1σ off the fundamental plane using the new coefficients listed in Appendix A, which are based on the work of Saulder et al (2013). Furthermore, all candidate galaxies can be found clearly within 3σ of the fundamental plane (see Fig.…”

Section: The Fundamental Planecontrasting

confidence: 54%

“…Here, σ 0 is typically about 10% higher than the measured value σ sdss (Saulder et al 2013). For the following calculations, one requires the luminosity distance D L , which is given by…”

Section: Methodsmentioning

confidence: 95%

“…follows the model of Chilingarian et al (2010), but with updated coefficients B i j from Saulder et al (2013). It requires the extinction-corrected magnitudes, m f 1 and m f 2 , of two different filters, f 1 and f 2 , and the observed redshift z obs .…”

Section: Methodsmentioning

confidence: 99%

“…B19 is indicated by a filled grey square. The black dashed line represents the fit on the red sequence performed in Saulder et al (2013) with the corresponding 3σ confidence intervals shown as solid red lines. Saulder et al (2013) in the g − r colour vs. the absolute z band magnitude plane.…”

Section: The Colour−magnitude Diagrammentioning

confidence: 99%

“…The black dashed line represents the fit on the red sequence performed in Saulder et al (2013) with the corresponding 3σ confidence intervals shown as solid red lines. Saulder et al (2013) in the g − r colour vs. the absolute z band magnitude plane. At a given absolute magnitude M z , the galaxies of our candidate sample are systematically redder than the average red sequence galaxy by about 0.05 mag in g − r. At the same time, except for two outliers, all galaxies are well within 3σ limits of the overall distribution, and there are only a few galaxies, which are blue than the average red sequence galaxy.…”

Section: The Colour−magnitude Diagrammentioning

confidence: 99%

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Dozens of compact and high velocity-dispersion, early-type galaxies in Sloan Digital Sky Survey

Saulder

Bosch

Mieske

2015

A&A

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Context. Passive galaxies at high redshift are much smaller than equally massive early types today. If this size evolution is caused by stochastic merging processes, then a small fraction of the compact galaxies should persist until today. Up to now it has not been possible to systematically identify the existence of such objects in Sloan Digital Sky Survey (SDSS). Aims. We aim at finding potential survivors of these compact galaxies in SDSS, as targets for more detailed follow-up observations. Methods. From the virial theorem, it is expected that for a given mass, compact galaxies have stellar velocity dispersion higher than the mean owing to their smaller sizes. Therefore velocity dispersion, coupled with size (or mass), is an appropriate method of selecting relics, independent of the stellar population properties. Based on these considerations, we designed a set of criteria the use the distribution of early-type galaxies from SDSS on the log 10 (R 0 )−log 10 (σ 0 ) plane to find the most extreme objects on it. We thus selected compact massive galaxy candidates by restricting them to high velocity dispersions σ 0 > 323.2 km s −1 and small sizes R 0 < 2.18 kpc. Results. We find 76 galaxies at 0.05 < z < 0.2, which have properties that are similar to the typical quiescent galaxies at high redshift. We discuss how these galaxies relate to average present-day early-type galaxies. We study how well these galaxies fit on well-known local universe relations of early-type galaxies, such as the fundamental plane, the red sequence, or mass-size relations. As expected from the selection criteria, the candidates are located in an extreme corner of the mass-size plane. However, they do not extend as deeply into the so-called zone of exclusion as some of the red nuggets found at high redshift, since they are a factor 2−3 less massive on a given intrinsic scale size. Several of our candidates are close to the size resolution limit of SDSS, but are not so small that they are classified as point sources. We find that our candidates are systematically offset on a scaling relation compared to the average early-type galaxies, but still within the general range of other early-type galaxies. Furthermore, our candidates are similar to the mass-size range expected for passive evolution of the red nuggets from their high redshift to the present. Conclusions. The 76 selected candidates form an appropriate set of objects for further follow-up observations. They do not constitute a separate population of peculiar galaxies, but form the extreme tail of a continuous distribution of early-type galaxies. We argue that selecting a high-velocity dispersion is the best way to find analogues of compact high redshift galaxies in the local universe.

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Section: The Fundamental Planecontrasting

confidence: 54%

“…Here, σ 0 is typically about 10% higher than the measured value σ sdss (Saulder et al 2013). For the following calculations, one requires the luminosity distance D L , which is given by…”

Section: Methodsmentioning

confidence: 95%

Section: Methodsmentioning

confidence: 99%

Section: The Colour−magnitude Diagrammentioning

confidence: 99%

Section: The Colour−magnitude Diagrammentioning

confidence: 99%

See 3 more Smart Citations

Dozens of compact and high velocity-dispersion, early-type galaxies in Sloan Digital Sky Survey

Saulder

Bosch

Mieske

2015

A&A

Self Cite

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Reconstructing the velocity field beyond the local universe

et al. 2014

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We present a maximum probability approach to reconstructing spatial maps of the peculiar velocity field at redshifts $z\sim0.1$, where the velocities have been measured from distance indicators (DI) such as $D_n-\sigma$ relations or Tully-Fisher. With the large statistical uncertainties associated with DIs, our reconstruction method aims to recover the underlying true peculiar velocity field by reducing these errors with the use of two physically motivated filtering prior terms. The first constructs an estimate of the velocity field derived from the galaxy over-density {\deltag} and the second makes use of the matter linear density power spectrum {\pk}. Using $N$-body simulations we find, with an SDSS-like sample ($N_{gal}\simeq33$ per deg$^2$), an average correlation coefficient value of $r=0.55\pm{0.02}$ between our reconstructed velocity field and that of the true velocity field from the simulation. However, with a suitably high number density of galaxies from the next generation surveys (e.g. $N_{gal}\simeq140$ per deg$^2$) we can achieve an average $r=0.70\pm{0.02}$ out to moderate redshifts $z\sim0.1$. This will prove useful for future tests of gravity, as these relatively deep maps are complementary to weak lensing maps at the same redshift.Comment: Accepted for publication in General Relativity and Gravitation (GRG

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