A Deep Proper Motion Catalog Within the Sloan Digital Sky Survey Footprint. Ii. The White Dwarf Luminosity Function

Munn, Jeffrey A.; Harris, Hugh C.; Hippel, Ted von; Kilic, Mukremin; Liebert, James; Williams, Kurtis A.; DeGennaro, Steven; Jeffery, Elizabeth; Dame, Kyra; Gianninas, A.; Brown, Warren R.

doi:10.3847/1538-3881/153/1/10

Cited by 40 publications

(63 citation statements)

References 73 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Hence, the latter survey significantly increases the number of stars beyond the turnover in the disk luminosity function, and it provides an excellent opportunity to disentangle the thin disk and thick disk luminosity functions. Figure 3 presents the disk luminosity function from Munn et al (2017) using the preferred disk model of Jurić et al (2008) with thin and thick disk scale heights of 300 and 900 pc, respectively, and a thick to thin disk ratio of 12%. As in the analysis of the 40 pc luminosity function, we only use stars with M 11 bol > mag in our fits.…”

Section: The Disk Luminosity Functionmentioning

confidence: 99%

“…Munn et al (2017) identified 8472 white dwarf candidates in this survey, and used 2839 stars with M 5.5 17 bol = -mag to create a disk white dwarf luminosity function. To avoid contamination from subdwarfs (at the low velocity end), they limited their disk sample to objects with v 40 120 tan = -km s −1 .…”

Section: The Disk Luminosity Functionmentioning

confidence: 99%

“…In Section 2 we describe the input model white dwarf luminosity functions, and in Section 3 we present an analysis of the local 40 pc white dwarf sample (Limoges et al 2015). In Section 4, we analyze the disk and halo luminosity functions from the deep proper motion survey of Munn et al (2014Munn et al ( , 2017 and present new age constraints for the three major components of the Galaxy. We compare these white dwarf age constraints with previous age measurements from the literature and highlight the next generation of surveys that will improve these age constraints in Section 5.…”

Section: Introductionmentioning

confidence: 99%

“…In addition, the proper motion survey of Munn et al (2014Munn et al ( , 2017 goes deep enough (r=21.5 mag) to uncover a sizable fraction of halo white dwarfs. Here we take advantage of this latter survey to constrain, for the first time, the ages of the thin disk, thick disk, and the halo from the same sample of white dwarfs.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

The Ages of the Thin Disk, Thick Disk, and the Halo from Nearby White Dwarfs

Kilic

Munn

Harris

et al. 2017

ApJ

Self Cite

145

127

View full text Add to dashboard Cite

We present a detailed analysis of the white dwarf luminosity functions derived from the local 40 pc sample and the deep proper motion catalog of Munn et al. Many previous studies have ignored the contribution of thick disk white dwarfs to the Galactic disk luminosity function, which results in an erroneous age measurement. We demonstrate that the ratio of thick/thin disk white dwarfs is roughly 20% in the local sample. Simultaneously fitting for both disk components, we derive ages of 6.8-7.0 Gyr for the thin disk and 8.7±0.1 Gyr for the thick disk from the local 40 pc sample. Similarly, we derive ages of 7.4-8.2 Gyr for the thin disk and 9.5-9.9 Gyr for the thick disk from the deep proper motion catalog, which shows no evidence of a deviation from a constant star formation rate in the past 2.5 Gyr. We constrain the time difference between the onset of star formation in the thin disk and the thick disk to be 1.6 0.4Gyr. The faint end of the luminosity function for the halo white dwarfs is less constrained, resulting in an age estimate of 12.5 3.4 -+Gyr for the Galactic inner halo. This is the first time that ages for all three major components of the Galaxy have been obtained from a sample of field white dwarfs that is large enough to contain significant numbers of disk and halo objects. The resultant ages agree reasonably well with the age estimates for the oldest open and globular clusters.

show abstract

Section: The Disk Luminosity Functionmentioning

confidence: 99%

Section: The Disk Luminosity Functionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The Ages of the Thin Disk, Thick Disk, and the Halo from Nearby White Dwarfs

Kilic

Munn

Harris

et al. 2017

ApJ

Self Cite

145

127

View full text Add to dashboard Cite

show abstract

“…[38,45] show that photometrically selected white dwarfs have a contamination around 40%. Even the ones selected also from proper motion by [46] show significant contamination by non-white dwarf objects, when spectra are available.…”

Section: Interacting Binariesmentioning

confidence: 99%

Pulsating white dwarfs

Romero

2017

EPJ Web Conf.

View full text Add to dashboard Cite

Abstract. The Sloan Digital Sky Survey has allowed us to increase the number of known white dwarfs by a factor of five and consequently the number of known pulsating white dwarfs also by a factor of five. It has also led to the discovery of new types of variable white dwarfs, as the variable hot DQs, and the pulsating Extremely Low Mass white dwarfs. With the Kepler Mission, it has been possible to discover new phenomena, the outbursts present in a few pulsating white dwarfs.

show abstract

White dwarfs as advanced physics laboratories. The axion case

Isern

2019

Proc. IAU

View full text Add to dashboard Cite

The shape of the luminosity function of white dwarfs (WDLF) is sensitive to the characteristic cooling time and, therefore, it can be used to test the existence of additional sources or sinks of energy such as those predicted by alternative physical theories. However, because of the degeneracy between the physical properties of white dwarfs and the properties of the Galaxy, the star formation history (SFH) and the IMF, it is almost always possible to explain any anomaly as an artifact introduced by the star formation rate. To circumvent this problem there are at least two possibilities, the analysis of the WDLF in populations with different stories, like disc and halo, and the search of effects not correlated with the SFH. These procedures are illustrated with the case of axions.

show abstract

A Deep Proper Motion Catalog Within the Sloan Digital Sky Survey Footprint. Ii. The White Dwarf Luminosity Function

Abstract: , respectively. We resolve the bump in the disk WDLF due to the onset of fully convective envelopes in WDs, and see indications of it in the halo WDLF as well.

Cited by 40 publications

References 73 publications

The Ages of the Thin Disk, Thick Disk, and the Halo from Nearby White Dwarfs

The Ages of the Thin Disk, Thick Disk, and the Halo from Nearby White Dwarfs

Pulsating white dwarfs

White dwarfs as advanced physics laboratories. The axion case

Contact Info

Product

Resources

About