GGD 27: X-Rays From a Massive Protostar With an Outflow

Pravdo, S. H.; Tsuboi, Y.; Suzuki, Yuichiro; Thompson, Tom; Rebull, L. M.

doi:10.1088/0004-637x/690/1/850

Cited by 17 publications

(30 citation statements)

References 62 publications

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“…Those identified by class based upon their IRAC fluxes include 3 Class 0-I, 13 Class II, 11 Class III, and 2 flat-spectrum stars, typical of star formation regions (e.g., Broos et al 2007;Getman et al 2007;Pravdo et al 2009, and many references therein). Three bright X-ray sources are located in the northwest cluster of enhanced mid-IR emission shown in Figures 2(a)-(d).…”

Section: Other X-ray Sourcesmentioning

confidence: 99%

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X-Rays From the Power Sources of the Cepheus a Star-Forming Region

Pravdo

Tsuboi

Uzawa

et al. 2009

ApJ

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We report an observation of X-ray emission from the exciting region of Cepheus A with the Chandra/ACIS instrument. What had been an unresolved X-ray source comprising the putative power sources is now resolved into at least three point-like sources, each with similar X-ray properties and differing radio and submillimeter properties. The sources are HW9, HW3c, and a new source that is undetected at other wavelengths "h10." They each have inferred X-ray luminosities 10 31 erg s −1 with hard spectra, T 10 7 K, and high low-energy absorption equivalent to tens to as much as a hundred magnitudes of visual absorption. The star usually assumed to be the most massive and energetic, HW2, is not detected with an upper limit about seven times lower than the detections. The X-rays may arise via thermal bremsstrahlung in diffuse emission regions associated with a gyrosynchrotron source for the radio emission, or they could arise from powerful stellar winds. We also analyzed the Spitzer/IRAC mid-IR observation from this star formation region and present the X-ray results and mid-IR classifications of the nearby stars. HH 168 is not as underluminous in X-rays as previously reported.

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Section: Other X-ray Sourcesmentioning

confidence: 99%

“…Leaving aside HH objects and other outflow sources, the only compact radio sources detected in the X-rays were MRR 12, 32, and 14 (Marti et al 1993). The first two were shown to be Class III PMS stars (Pravdo et al 2009). In Cepheus A east, none of the classified mid-IR sources is a radio source.…”

Section: Comparative Taxonomymentioning

confidence: 99%

X-Rays From the Power Sources of the Cepheus a Star-Forming Region

Pravdo

Tsuboi

Uzawa

et al. 2009

ApJ

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“…There is another site of massive star formation, the core MM2, located 7 ′′ (∼ 10000 au) northeast of MM1. These two massive protostellar sites are surrounded by a cluster of infrared and X-ray sources (e. g., Aspin et al 1994;Pravdo et al 2004Pravdo et al , 2009Qiu et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1

Busquet

Girart

Estalella

et al. 2019

A&A

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Context. Most stars form in clusters, and thus it is important to characterize the protostellar disk population in dense environments to assess whether the environment plays a role in the subsequent evolution; specifically, whether planet formation is altered with respect to more isolated stars formed in dark clouds. Aims. Investigate the properties of the protostellar disks in the GGD 27 cluster and compare them with those obtained from disks formed in nearby regions. Methods. We used ALMA to observe the star-forming region GGD 27 at 1.14 mm with an unprecedented angular resolution, 40 mas (∼ 56 au) and sensitivity (∼ 0.002 M ⊙ ). Results.We detected a cluster of 25 continuum sources, most of which are likely tracing disks around Class 0/I protostars. Excluding the two most massive objects, disks masses are in the range 0.003-0.05 M ⊙ . The analysis of the cluster properties indicates that GGD 27 displays moderate subclustering. This result combined with the dynamical timescale of the radio jet (∼ 10 4 years) suggests the youthfulness of the cluster. The lack of disk mass segregation signatures may support this too. We found a clear paucity of disks with R disk > 100 au. The median value of the radius is 34 au, smaller than the median of 92 au for Taurus but comparable to the value found in Ophiuchus and in the Orion Nebula Cluster. In GGD 27 there is no evidence of a distance-dependent disk mass distribution (i. e., disk mass depletion due to external photoevaporation), most likely due to the cluster youth. There is a clear deficit of disks for distances < 0.02 pc. Only for distances > 0.04 pc stars can form larger and more massive disks, suggesting that dynamical interactions far from the cluster center are weaker, although the small disks found could be the result of disk truncation. This work demonstrates the potential to characterize disks from low-mass YSOs in distant and massive (still deeply embedded) clustered environments.

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“…In low-mass protostars, models show that episodes of magnetic reconnection between the disk material and the protostar lead to X-ray emission and possibly even gammaray emission (del Valle et al 2011). The former might be also occuring in high-mass protostars (Pravdo et al 2009). Thus, the detected X-ray radiation in IRAS 16547−4247 may come from the central protostar alone, from the RS, or be the sum of the contribution of the RS and the central source.…”

Section: Connection With X-ray Observationsmentioning

confidence: 98%

Studying the non-thermal lobes of IRAS 16547−4247 through a multi-wavelength approach

Munar-Adrover¹,

Bosch‐Ramon²,

Paredes³

et al. 2013

A&A

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In recent years, massive protostars have turned out to be a possible population of high-energy emitters. Among the best candidates is IRAS 16547-4247, a protostar that presents a powerful outflow with clear signatures of interaction with its environment. This source has been revealed to be a potential high-energy source because it displays non-thermal radio emission of synchrotron origin, which is evidence of relativistic particles. To improve our understanding of IRAS 16547-4247 as a high-energy source, we analyzed XMM-Newton archival data and found that IRAS 16547−4247 is a hard X-ray source. We discuss these results in the context of a refined one-zone model and previous radio observations. From our study we find that it may be difficult to explain the X-ray emission as non-thermal radiation coming from the interaction region, but it might be produced by thermal Bremsstrahlung (plus photo-electric absorption) by a fast shock at the jet end. In the high-energy range, the source might be detectable by the present generation of Cherenkov telescopes, and may eventually be detected by Fermi in the GeV range.

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GGD 27: X-Rays From a Massive Protostar With an Outflow

Cited by 17 publications

References 62 publications

X-Rays From the Power Sources of the Cepheus a Star-Forming Region

X-Rays From the Power Sources of the Cepheus a Star-Forming Region

Unveiling a cluster of protostellar disks around the massive protostar GGD 27 MM1

Studying the non-thermal lobes of IRAS 16547−4247 through a multi-wavelength approach

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