Observational constraints for the circumstellar disk of the B[e] star CPD−52 9243

Cidale, L. S.; Fernandes, M. Borges; Andruchow, I.; Arias, María Laura; Kraus, M.; Chesneau, O.; Kanaan, S.; Curé, M.; Wit, W. J. de; Muratore, M. F.

doi:10.1051/0004-6361/201220120

Cited by 30 publications

(53 citation statements)

References 29 publications

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“…As CO band emission typically arises from the inner rim/edge of the molecular disk region, the fact that our CO model temperatures are all much cooler than the dissociation temperature of 5000 K indicates that the material may be located in a detached disk structure, as opposed to a disk that reaches the stellar surface as suggested by the model of Zickgraf et al (1986). Such behavior has recently been reported in other studies Liermann et al 2010;Wheelwright et al 2012;Cidale et al 2012).…”

Section: Model Resultssupporting

confidence: 85%

Probing the ejecta of evolved massive stars in transition

Oksala

Kraus

Cidale

et al. 2013

A&A

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139

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Massive evolved stars in transition phases, such as luminous blue variables (LBVs), B[e] supergiants (B[e]SGs), and yellow hypergiants (YHGs), are not well understood, and yet crucial steps in determining accurate stellar and galactic evolution models. The circumstellar environments of these stars reveal their mass-loss history, identifying clues to both their individual evolutionary status and the connection between objects of different phases. Here we present a survey of 25 such evolved massive stars (16 B[e]SGs, 6 LBVs, 2 YHGs, and 1 Peculiar Oe star), observed in the K-band with the Spectrograph for INtegral Field Observation in the Near-Infrared (SINFONI; R = 4500) on the ESO VLT UT4 8 m telescope. The sample can be split into two categories based on spectral morphology: one group includes all of the B[e]SGs, the Peculiar Oe star, and two of the LBVs, while the other includes the YHGs and the rest of the LBVs. The difference in LBV spectral appearance is due to some objects being in a quiescent phase and some objects being in an active or outburst phase. CO emission features are found in 13 of our targets, with first time detections for MWC 137, LHA 120-S 35, and LHA 115-S 65. From model fits to the CO band heads, the emitting regions appear to be detached from the stellar surface. Each star with 12 CO features also shows 13 CO emission, signaling an evolved nature. Based on the level of 13 C enrichment, we conclude that many of the B[e]SGs are likely in a pre-Red Supergiant phase of their evolution. There appears to be a lower luminosity limit of log L/L = 5.0 below which CO is not detected. The lack of CO features in several high luminosity B[e]SGs and variability in others suggests that they may in fact be LBV candidates, strengthening the connection between these two very similar transition phases.

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Section: Model Resultssupporting

confidence: 85%

Probing the ejecta of evolved massive stars in transition

Oksala

Kraus

Cidale

et al. 2013

A&A

Self Cite

139

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“…The derived CO parameters (i.e., temperature and column density) are similar to those found for other B[e]SGs such as LHA 120-S 12 and LHA 120-S 73 in the Large Magellanic Cloud , LHA 115-S 65 in the Small Magellanic Cloud (Oksala et al 2012), and CPD-52 9243 (Cidale et al 2012) and MWC 349A (Kraus et al 2000) in the Galaxy. Only one Galactic object, HD 327083, seems to be extreme in the sense that its disk, studied by Wheelwright et al (2012), has the coolest (T CO = 1721 ± 540 K) and densest (N CO = (0.4 ± 1.8) × 10 24 cm −2 ) CO gas.…”

Section: Resultssupporting

confidence: 80%

“…Former calculations of CO emission from a disk revealed that it is sufficient to consider the innermost ring of gas with a constant temperature, column density, and rotation velocity (e.g., Kraus 2009;Liermann et al 2010;Cidale et al 2012).…”

Section: Resultsmentioning

confidence: 99%

Molecular emission from GG Carinae’s circumbinary disk

Kraus

Oksala

Nickeler

et al. 2012

A&A

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Context. The appearance of the B[e] phenomenon in evolved massive stars such as B [e] supergiants is still a mystery. While these stars are generally found to have disks that are cool and dense enough for efficient molecule and dust condensation, the origin of the disk material is still unclear. Aims. We aim at studying the kinematics and origin of the disk in the eccentric binary system GG Car, whose primary component is proposed to be a B[e] supergiant. Methods. Based on medium-and high-resolution near-infrared spectra we analyzed the CO-band emission detected from GG Car. The complete CO-band structure delivers information on the density and temperature of the emitting region, and the detectable 13 CO bands allow us to constrain the evolutionary phase. In addition, the kinematics of the CO gas can be extracted from the shape of the first 12 CO band head. Results. We find that the CO gas is located in a ring surrounding the eccentric binary system, and its kinematics agrees with Keplerian rotation with a velocity, projected to the line of sight, of 80 ± 1 km s −1 . The CO ring has a column density of (5 ± 3) × 10 21 cm −2 and a temperature of 3200 ± 500 K. In addition, the material is chemically enriched in 13 C, which agrees with the primary component being slightly evolved off the main sequence. We discuss two possible scenarios for the origin of the circumbinary disk: (i) nonconservative Roche lobe overflow; and (ii) the possibility that the progenitor of the primary component could have been a classical Be star. Neither can be firmly excluded, but for Roche lobe overflow to occur, a combination of stellar and orbital parameter extrema would be required.

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“…We note that our derived IR luminosity is a lower limit of the total luminosity of the heating source, since we are only sensitive to warm (∼600 K) dust at 3.6 and 4.5 μm. Remarkably, the equilibrium temperature radius of surrounding dust (~-R 10 20 au eq ) matches the inner edge radii of spatially resolved galactic sgB[e] disks: 30 au for CPD-52 9243 (Cidale et al 2012) and~-20 30 au for MWC 300 (Wang et al 2012). X-1 is therefore a member of an emerging class of luminous X-ray sources with donor stars that resemble sgB[e] stars such as IGR J16318-4848 (Filliatre & Chaty 2004), GX 301-2 (Servillat et al 2014), and SN2010 da (Binder et al 2016;Lau et al 2016;Villar et al 2016).…”

Section: X-1 Donor: a Supergiant B[e] Star?mentioning

confidence: 67%

First Detection of Mid-infrared Variability from an Ultraluminous X-Ray Source Holmberg II X-1

Lau

Heida

Kasliwal

et al. 2017

ApJL

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We present mid-infrared (IR) light curves of the Ultraluminous X-ray Source (ULX) Holmberg II X-1 from observations taken between 2014 January 13 and 2017 January 5 with the Spitzer Space Telescope at 3.6 and 4.5 μm in the Spitzer Infrared Intensive Transients Survey. The mid-IR light curves, which reveal the first detection of mid-IR variability from a ULX, is determined to arise primarily from dust emission rather than from a jet or an accretion disk outflow. We derived the evolution of the dust temperature (~-T 600 800, and equilibrium temperature radius (~-R 10 20 au eq ). A comparison of X-1 with a sample of spectroscopically identified massive stars in the Large Magellanic Cloud on a mid-IR color-magnitude diagram suggests that the mass donor in X-1 is a supergiant (sg) B[e]-star. The sgB[e]-interpretation is consistent with the derived dust properties and the presence of the [Fe II] (l m = 1.644 m) emission line revealed from previous near-IR studies of X-1. We attribute the mid-IR variability of X-1 to the increased heating of dust located in a circumbinary torus. It is unclear what physical processes are responsible for the increased dust heating; however, it does not appear to be associated with the X-ray flux from the ULX, given the constant X-ray luminosities provided by serendipitous, near-contemporaneous X-ray observations around the first mid-IR variability event in 2014. Our results highlight the importance of mid-IR observations of luminous X-ray sources traditionally studied at X-ray and radio wavelengths.

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Observational constraints for the circumstellar disk of the B[e] star CPD−52 9243

Cited by 30 publications

References 29 publications

Probing the ejecta of evolved massive stars in transition

Probing the ejecta of evolved massive stars in transition

Molecular emission from GG Carinae’s circumbinary disk

First Detection of Mid-infrared Variability from an Ultraluminous X-Ray Source Holmberg II X-1

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