Absolute magnitudes of OB and Be stars based on Hipparcos parallaxes - III

Wegner, W.

doi:10.1111/j.1365-2966.2006.11265.x

Cited by 40 publications

(36 citation statements)

References 17 publications

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“…3.2. The distance modulus was determined to μ = 13.6 ± 0.8 mag by minimizing the difference in M V for all stars to literature values for the respective spectral types (Wegner 2006(Wegner , 2007. The errors in both color and absolute magnitude are large because of the high uncertainties in the interstellar medium extinction and the uncertainties in the spectral classification (see Sects.…”

Section: The Extinction To Mwc 137 Via the Spectral Energy Distributimentioning

confidence: 99%

VLT/MUSE discovers a jet from the evolved B[e] star MWC 137

Mehner

Wit

Groh

et al. 2015

A&A

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Aims. Not all stars exhibiting the optical spectral characteristics of B [e] stars are in the same evolutionary stage. The Galactic B[e] star MWC 137 is a prime example of an object with uncertain classification, where previous work has suggested either a pre-or a postmain sequence classification. Our goal is to settle this debate and provide a reliable evolutionary classification. Methods. Integral field spectrograph observations with the Very Large Telescope Multi Unit Spectroscopic Explorer (VLT MUSE) of the cluster SH 2-266 are used to analyze the nature of MWC 137. Results. A collimated outflow is discovered that is geometrically centered on MWC 137. The central position of MWC 137 in the cluster SH 2-266 within the larger nebula suggests strongly that it is a member of this cluster and that it is the origin of both the nebula and the newly discovered jet. Comparison of the color-magnitude diagram of the brightest cluster stars with stellar evolutionary models results in a distance of about 5.2 ± 1.4 kpc. We estimate that the cluster is at least 3 Myr old. The jet emanates from MWC 137 at a position angle of 18-20• . The jet extends over 66 (1.7 pc) projected on the plane of the sky, shows several knots, and has electron densities of about 10 3 cm −1 and projected velocities of up to ±450 km s −1 . From the Balmer emission line decrement of the diffuse intracluster nebulosity, we determine E(B-V) = 1.4 mag for the inner 1 cluster region. The spectral energy distribution of the brightest cluster stars yields a slightly lower extinction of E(B-V) ∼ 1.2 mag for the inner region and E(B-V) ∼ 0.4-0.8 mag for the outer region. The extinction toward MWC 137 is estimated to be E(B-V) ∼ 1.8 mag (A V ∼ 5.6 mag). Conclusions. Our analysis of the optical and near-infrared color-magnitude and color-color diagrams suggests a post-main sequence stage for MWC 137. The existence of a jet in this object implies the presence of an accretion disk. Several possibilities for MWC 137's nature and the origin of its jet are discussed: e.g., the presence of a companion and a merger event.

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Section: The Extinction To Mwc 137 Via the Spectral Energy Distributimentioning

confidence: 99%

VLT/MUSE discovers a jet from the evolved B[e] star MWC 137

Mehner

Wit

Groh

et al. 2015

A&A

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“…Moffat & Vogt (1973) cite V = 8.41, B − V = 0.21, and U − B = −0.63 for HD 108719. According to Wegner (2007), the absolute magnitude of a B1 III, B1 II, and B1 Ib star is M V = −3.71, −4.27, and −4.65, respectively. These values disagree with the estimates of Schmidt-Kaler (1982), namely M V = −4.4, −5.4, and −5.8.…”

Section: Cpd−64 1943 and Hd 108719mentioning

confidence: 99%

Investigating potential planetary nebula/cluster pairs

Bidin

Majaess²,

Bonatto

et al. 2014

A&A

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Context. Fundamental parameters characterizing the end-state of intermediate-mass stars may be constrained by discovering planetary nebulae (PNe) in open clusters (OCs). Cluster membership may be exploited to establish the distance, luminosity, age, and physical size for PNe, and the intrinsic luminosity and mass of its central star. Aims. Four potential PN-OC associations were investigated to assess the cluster membership for the PNe. Methods. Radial velocities were measured from intermediate-resolution optical spectra, complemented with previous estimates in the literature. When the radial velocity study supported the PN/OC association, we analyzed whether other parameters (e.g., age, distance, reddening, central star brightness) were consistent with this conclusion. Results. Our measurements imply that the PNe VBe 3 and HeFa 1 are not members of the OCs NGC 5999 and NGC 6067, respectively, and that they very likely belong to the background bulge population. Conversely, consistent radial velocities indicate that NGC 2452/NGC 2453 could be associated, but our results are not conclusive so additional observations are warranted. Finally, we demonstrate that all the available information point to He 2-86 being a young, highly internally obscured PN member of NGC 4463. New near-infrared photometry acquired via the Vista Variables in the Via Lactea ESO public survey was used in tandem with existing UBV photometry to measure the distance, reddening, and age of NGC 4463, finding d = 1.55 ± 0.10 kpc, E(B − V) = 0.41 ± 0.02, and τ = 65 ± 10 Myr, respectively. The same values should be adopted for the PN if the proposed cluster membership is confirmed.

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“…The reverse is also true: if A Ks,test < A Ks,GC and D test > D GC , then such a star cannot be a counterpart either. The absolute magnitudes of stars of various classes M Ks,test were taken from Wegner (2007Wegner ( , 2014.…”

Section: The Infrared Band V V V Survey Resultsmentioning

confidence: 99%

IGR J17463-2854, a possible symbiotic binary system in the galactic center region

2015

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This paper is devoted to determining the nature of the hard X-ray source IGR J17463-2854 located toward the Galactic bulge. Using data from the INTEGRAL and Chandra X-ray observatories, we show that five point X-ray sources with approximately identical fluxes in the 2-10 keV energy band are detected in the error circle of the object under study. In addition, significant absorption at low energies has been detected in the spectra of all these sources. Based on data from the VVV (VISTA/ESO) infrared Galactic Bulge Survey, we have unambiguously identified three of the five sources, determined the J, H and K magnitudes of the corresponding stars, and obtained upper limits on the fluxes for the remaining two sources. Analysis of the color-magnitude diagrams has shown that one of these objects most likely belongs to a class of rarely encountered objects, symbiotic binary systems (several tens are known with certainty), i.e., low-mass binary systems consisting of a white dwarf and a red giant. Note that all our results were obtained using improved absorption values and an extinction law differing in this direction from the standard one.

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Absolute magnitudes of OB and Be stars based on Hipparcos parallaxes - III

Cited by 40 publications

References 17 publications

VLT/MUSE discovers a jet from the evolved B[e] star MWC 137

VLT/MUSE discovers a jet from the evolved B[e] star MWC 137

Investigating potential planetary nebula/cluster pairs

IGR J17463-2854, a possible symbiotic binary system in the galactic center region

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