Local Interstellar Reddening

Gottlieb, D. M.; Upson, W. L.

doi:10.1086/150101

Cited by 25 publications

(17 citation statements)

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“…Racine (1968) determined a shorter distance of 135±10pc from the photometry of bright stars associated with reflection nebulae. On the other hand, Gottlieb & Upson (1969) obtained a somewhat larger distance of 150pc based on the reddening turn-on method. Later, Straizys & Meistas (1980) investigated the area around the dark clouds L1538, L1528, L1521, and L1495 from the Lynds catalog (Lynds 1962) using a similar approach and concluded that they extend from 140 to 175pc.…”

Section: Introductionmentioning

confidence: 90%

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

Galli

Loinard

Ortiz-León

et al. 2018

ApJ

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We present new trigonometric parallaxes and proper motions of young stellar objects in the Taurus molecular cloud complex from observations collected with the Very Long Baseline Array as part of the Gould's Belt Distances Survey. We detected 26 young stellar objects and derived trigonometric parallaxes for 18 stars with an accuracy of 0.3% to a few percent. We modeled the orbits of six binaries and determined the dynamical masses of the individual components in four of these systems (V1023 Tau, T Tau S, V807 Tau, and V1000 Tau). Our results are consistent with the first trigonometric parallaxes delivered by the Gaia satellite and reveal the existence of significant depth effects. We find that the central portion of the dark cloud Lynds1495 is located at d= 129.5±0.3 pc, while the B216 clump in the filamentary structure connected to it is at d=158.1±1.2 pc. The closest and remotest stars in our sample are located at d=126.6±1.7 pc and d=162.7±0.8 pc, yielding a distance difference of about 36pc. We also provide a new distance estimate for HLTau that was recently imaged. Finally, we compute the spatial velocity of the stars with published radial velocity and investigate the kinematic properties of the various clouds and gas structures in this region.

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Section: Introductionmentioning

confidence: 90%

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

Galli

Loinard

Ortiz-León

et al. 2018

ApJ

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“…A comprehensive discussion of distance estimates for the Taurus-Auriga SFR (Greenstein 1937;McCuskey 1939;Gottlieb & Upson 1969;Racine 1968) can be found in Elias (1978), who concluded that the most likely value of the distance is about 140 Ϯ 20 pc.…”

Section: Taurus-aurigamentioning

confidence: 99%

Hipparcos observations of pre-main-sequence stars

Wichmann¹,

Bastian

Krautter³

et al. 1998

Monthly Notices of the Royal Astronomical Society

174

163

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We present first results of Hipparcos observations of nearby low‐mass pre‐main‐sequence (PMS) stars (T Tauri and Herbig Ae/Be stars). The data obtained by Hipparcos allow us to derive weighted mean parallaxes for three major nearby star‐forming regions (SFRs), Lupus, Chamaeleon I and Taurus–Auriga. Furthermore, results on the isolated objects AB Dor and TW Hya are presented. Finally, we discuss the evolutionary status of Herbig Ae/Be (HAEBE) stars on the basis of Hipparcos results.

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“…• ) have on average a colour excess per kiloparsec of E(B − V) = 0.05 ± 0.05 mag kpc −1 (Gottlieb & Upson 1969). Therefore, the colour excesses E(J−K) and E(B−R) are negligible compared to the optical and infrared magnitude uncertainties (Schild 1977).…”

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confidence: 94%

X-ray source population study of the starburst galaxy M 83 withXMM-Newton

Ducci

Sasaki

Haberl

et al. 2013

A&A

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Aims. We present the results obtained from the analysis of three XMM-Newton observations of M 83. The aims of the paper are studying the X-ray source populations in M 83 and calculating the X-ray luminosity functions of X-ray binaries for different regions of the galaxy. Methods. We detected 189 sources in the XMM-Newton field of view in the energy range of 0.2-12 keV. We constrained their nature by means of spectral analysis, hardness ratios, studies of the X-ray variability, and cross-correlations with catalogues in X-ray, optical, infrared, and radio wavelengths. Results. We identified and classified 12 background objects, five foreground stars, two X-ray binaries, one supernova remnant candidate, one super-soft source candidate and one ultra-luminous X-ray source. Among these sources, we classified for the first time three active galactic nuclei (AGN) candidates. We derived X-ray luminosity functions of the X-ray sources in M 83 in the 2-10 keV energy range, within and outside the D 25 ellipse, correcting the total X-ray luminosity function for incompleteness and subtracting the AGN contribution. The X-ray luminosity function inside the D 25 ellipse is consistent with that previously observed by Chandra.The Kolmogorov-Smirnov test shows that the X-ray luminosity function of the outer disc and the AGN luminosity distribution are uncorrelated with a probability of ∼99.3%. We also found that the X-ray sources detected outside the D 25 ellipse and the uniform spatial distribution of AGNs are spatially uncorrelated with a significance of 99.5%. We interpret these results as an indication that part of the observed X-ray sources are X-ray binaries in the outer disc of M 83.

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Local Interstellar Reddening

Cited by 25 publications

References 0 publications

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

The Gould's Belt Distances Survey (GOBELINS). IV. Distance, Depth, and Kinematics of the Taurus Star-forming Region

Hipparcos observations of pre-main-sequence stars

X-ray source population study of the starburst galaxy M 83 withXMM-Newton

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