The PPMXL Catalog of Positions and Proper Motions on the Icrs. Combining USNO-B1.0 and the Two Micron All Sky Survey (2mass)

Roêser, S.; Demleitner, Markus; Schilbach, E.

doi:10.1088/0004-6256/139/6/2440

Cited by 807 publications

(822 citation statements)

References 16 publications

Supporting

Mentioning

805

Contrasting

Unclassified

Order By: Relevance

“…The colours and magnitudes of the reference stars yield a 1.6 mas correction due to the finite distance of the stars forming the reference frame, so our absolute parallax estimate is 9.9±1.3 mas, which on face value gives a distance to SDSS J1257+5428 of ∼ 101±15 pc. The proper motion relative to the reference frame is modest, [µX , µY ] = [−45, +9] mas yr −1 ; the PPMXL catalogue (Roeser et al 2010) gives [−41.0, +11.8] mas yr −1 , in very good agreement. Thorstensen (2003) describes a Bayesian procedure for estimating a distance by combining parallax information with proper motion (interpreted using an assumed space-velocity distribution) and with photometric distances.…”

Section: Parallax Observationsmentioning

confidence: 84%

A double white dwarf with a paradoxical origin?

Bours¹,

Marsh²,

Gänsicke³

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present Hubble Space Telescope UV spectra of the 4.6 h period double white dwarf SDSS J125733.63+542850.5. Combined with Sloan Digital Sky Survey optical data, these reveal that the massive white dwarf (secondary) has an effective temperature T 2 = 13030 ± 70 ± 150 K and a surface gravity log g 2 = 8.73 ± 0.05 ± 0.05 (statistical and systematic uncertainties respectively), leading to a mass of M 2 = 1.06 M ⊙ . The temperature of the extremely low-mass white dwarf (primary) is substantially lower at T 1 = 6400 ± 37 ± 50 K, while its surface gravity is poorly constrained by the data. The relative flux contribution of the two white dwarfs across the spectrum provides a radius ratio of R 1 /R 2 ≃ 4.2, which, together with evolutionary models, allows us to calculate the cooling ages. The secondary massive white dwarf has a cooling age of ∼ 1 Gyr, while that of the primary low-mass white dwarf is likely to be much longer, possibly 5 Gyrs, depending on its mass and the strength of chemical diffusion. These results unexpectedly suggest that the low-mass white dwarf formed long before the massive white dwarf, a puzzling discovery which poses a paradox for binary evolution.

show abstract

Section: Parallax Observationsmentioning

confidence: 84%

A double white dwarf with a paradoxical origin?

Bours¹,

Marsh²,

Gänsicke³

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…The astrophysical parameters of the investigated cluster have been estimated using the PPMXL Catalogue of Roeser et al (2010). It is combining the USNO-B1.0 proper motion of Monet et al (2003) and NIR JHK s pass-band of 2MASS Point Sources of Cutri et al (2003).…”

Section: Ppmxl Data Extraction and Preparationmentioning

confidence: 99%

“…(pm α cos δ) and (pm δ) mas yr −1 . According to Roeser et al (2010), the stars with proper motion uncertainties ≥ 4.0 mas yr −1 have been removed. Also, in this context, the stars with observational uncertainties ≥ 0.20 mag are excluded, and the photometric completeness limit is applied on the photometric pass-band 2MASS data to avoid the over-sampling at the lower parts of the cluster's colour magnitude diagrams (CMDs) (cf.…”

mentioning

confidence: 99%

PPMXL photometric analysis of three open cluster candidates

Tadross¹

2012

New Astronomy

View full text Add to dashboard Cite

We present here the astrophysical parameters of three stellar open cluster candidates using PPMXL 1 database. In this study, the main photometric, astrometry and statistical parameters of Ruprecht 13, Ruprecht 16 and Ruprecht 24 are estimated for the first time.Keywords: open clusters and associations -individual: Ruprecht (13, 16, 24) -astrometry -Stars -astronomical databases: catalogues. PACS: 91.10. Lh, 95.80.+p, 95.85.Jq, 97.10.Zr, 98.20.Di Open star clusters (OCs) play an important role in studying the formation and evolution of the Galactic disk and the stellar evolution as well. The fundamental physical parameters of OCs, e.g. distance, reddening, age, and metallicity are necessary for studying the Galactic disk. The strong interest of OCs results come from their fundamental properties. Among the 1787 currently OCs, more than half of them have been poorly studied or even unstudied up to now, Piatti et al. (2011). Thus the current paper is a part of our continuation series whose goal is to obtain the main astrophysical properties of previously unstudied OCs using modern databases. The most important thing for using PPMXL database lies in containing the positions, proper motions of USNO-B1.0 2 and the Near Infrared (NIR) photometry of the Two Micron All Sky Survey (2MASS) 3 , which let it be the powerful detection of the star clusters behind the hydrogen thick clouds on the Galactic plane.Our candidates are selected from among the unstudied OCs of Ruprecht catalogue (hereafter, Ru 13, Ru 16, and Ru 24). They are lying in the third quarter of Galactic longitude and close to the Galactic plane. The only available information about these clusters are the coordinates and the apparent diame- * Tel/Fax: +202 25560645/ +202 25548020 Table 1. The quality of the data is taken into account and the physical properties of each cluster are estimated by applying the same methodology. This paper is organized as follows. PPMXL data extraction and preparation are presented in Section 2, while the data analysis and parameters estimations are described in Sections 3. Finally, the conclusion is devoted to Section 4. PPMXL Data Extraction and preparationThe astrophysical parameters of the investigated cluster have been estimated using the PPMXL Catalogue of Roeser et al. (2010). It is combining the USNO-B1.0 proper motion of Monet et al. (2003) and NIR JHK s pass-band of 2MASS Point Sources of Cutri et al. (2003). USNO-B1.0 is a very useful catalogue, which gives us an opportunity to distinguish between the members and background/field stars. While, NIR 2MASS photometry provides J (1.25µm), H (1.65µm), and K s (2.17µm) band photometry for millions of galaxies and nearly a half-billion stars (Carpenter, 2001). This survey has proven to be a powerful tool in the analysis of the structure and stellar content of open clusters . The photometric uncertainty of the 2MASS data is less than 0.155 at K s ∼ 16.5 magnitude which is the photometric completeness for stars with |b| > 25 o , Skrutskie et al. (2006).It is noted th...

show abstract

“…PPMXL (Roeser et al, 2010) is a catalogue of positions, proper motions, 2MASS and optical photometry of 900 million stars and galaxies. The Two Micron All Sky Survey (2MASS; Skrutskie et al (2006)) uses two highly-automated 1.3-m telescopes (one at Mt.…”

Section: Introductionmentioning

confidence: 99%

Basic parameters of open star clusters DOLIDZE 14 and NGC 110 in infrared bands

Joshi

et al. 2015

New Astronomy

View full text Add to dashboard Cite

The basic physical parameters of a poorly studied open cluster NGC 110 and an unstudied open cluster DOLIDZE 14 are estimated in the present study using the archival P P MXL and W ISE catalogues. The radius of both the clusters are estimated by fitting the modified King's empirical model on their stellar density profiles. The other basic parameters of the clusters such as distance, reddening, and age are obtained by visual fitting of the Marigo's solar metallicity isochrone on their IR colour-magnitude diagrams (CMDs). The mean-proper motion of the clusters are estimated through the individual proper motion of probable members identified through the dynamical and statistical methods. The archival catalogues (JHKW 1 W 2 ) are constructed for both the clusters by compiling the extracted data from the P P MXL and W ISE catalogues. The various colour-excesses, such as E(J −H), E(H −K) and E(W 1 − W 2 ), are estimated using the best fit theoretical isochrone on the (J − H) − H, (H − K) − H and (W 1 − W 2 ) − H CMDs, respectively. The ratios of various infrared colours of the clusters are obtained through their two-colour diagrams. We also identify the most probable members in these clusters by estimating spatial, kinematic and spatio-kinematic probabilities of stars within the cluster. A correlation between the E(H −K) and E(W 1 −W 2 ) is also established.

show abstract

The PPMXL Catalog of Positions and Proper Motions on the Icrs. Combining USNO-B1.0 and the Two Micron All Sky Survey (2mass)

Cited by 807 publications

References 16 publications

A double white dwarf with a paradoxical origin?

A double white dwarf with a paradoxical origin?

PPMXL photometric analysis of three open cluster candidates

Basic parameters of open star clusters DOLIDZE 14 and NGC 110 in infrared bands

Contact Info

Product

Resources

About