Post‐Outburst Infrared Spectra of V1647 Ori, the Illuminating Star of McNeil’s Nebula

Gibb, E. L.; Rettig, T. W.; Brittain, S.; Wasikowski, D. A.; Simon, Theodore; Vacca, William D.; Cushing, Michael C.; Kulesa, Craig

doi:10.1086/500448

Cited by 21 publications

(56 citation statements)

References 23 publications

(40 reference statements)

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“…The spectrum also resembles those of the outbursting protostars V1647 Ori, PTF 10nvg, and PV Cephei (Gibb et al 2006;Covey et al 2011;Hillenbrand et al 2013;Caratti o Garatti et al 2013, see Fig. 11).…”

Section: Line Identificationsupporting

confidence: 52%

“…The characteristics of the HBe component during the 2008 outburst are not fully typical of EX Or objects and outbursting stars. The variation in the NIR continuum slope (colors) of the HBe with respect to the absolute NIR flux is anticorrelated with the one of V1647 Ori, PV Cep, or V1118 Ori (Gibb et al 2006;Lorenzetti et al 2009;Giannini et al 2016a). The emission lines of these four reference objects are correlated with their overall NIR brightness (outburst or quiescence) like Z CMa, based on the current stage of observations (temporal baseline, frequency of the measurements) of all those systems.…”

Section: Origins Of the Outburst: Extinction Or Accretion?mentioning

confidence: 89%

“…We propose an identification of most of the lines, for which we rely on analogies between our spectrum and those of several young embedded targets found in the literature (Kelly et al 1994;Greene & Lada 1996;Nisini et al 2005;Gibb et al 2006;Antoniucci et al 2008;Connelley & Greene 2010;Covey et al 2011;Kóspál et al 2011b;Caratti o Garatti et al 2013;Cooper et al 2013). We completed and double-checked the identifica-2 The tool can be downloaded at http//fuse.pha.jhu.edu/analysis/fuse idl tools.html tion using three databases for atomic and ionic transitions 3,4,5 .…”

Section: Line Identificationmentioning

confidence: 99%

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The 2008 outburst in the young stellar system Z CMa

Bonnefoy

Chauvin

Dougados

et al. 2017

A&A

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Context. Z CMa is a complex pre-main sequence binary with a current separation of 110 mas, known to consist of an FU Orionis star (SE component) and an embedded Herbig Be star (NW component). Although it represents a well-studied and characterized system, the origin of photometric variabilities, the component properties, and the physical configuration of the system remain mostly unknown. Aims. Immediately when the late-2008 outburst of Z CMa was announced to the community, we initiated a high angular resolution imaging campaign aimed at characterizing the outburst state of both components of the system in the near-infrared. Methods. We used the VLT/NACO and the Keck/NIRC2 near-infrared adaptive optics instrument to monitor the astrometric position and the near-infrared photometry of the Z CMa components during the outburst phase and one year after. The VLT/SINFONI and Keck/OSIRIS integral field spectroscrographs were in addition used to characterize for the first time the resolved spectral properties of the FU Orionis and the Herbig Be component during and after the outburst. Results. We confirm that the NW star dominates the system flux in the 1.1-3.8 µm range and is responsible for the photometric outburst. We extract the first medium-resolution (R∼2000-4000) near-infrared (1.1-2.4 µm) spectra of the individual components. The SE component has a spectrum typical of FU Orionis objects. The NW component spectrum is characteristic of embedded outbursting protostars and EX Or objects. It displays numerous emission lines whose intensity correlates with the system activity. In particular, we find a correlation between the Brγ equivalent width and the system brightness. The bluing of the continuum of the NW component along with the absolute flux and color-variation of the system during the outburst suggests that the outburst was caused by a complex interplay between a variation of the extinction in the line of sight of the NW component on one hand, and the emission of shocked regions close to the NW component on the other. We confirm the recently reported wiggling of the SE component jet from [FeII] line emission. We find a point-like structure associated with a peak emission at 2.098µm coincidental with the clump or arm seen in broadband polarization differential imaging as well as additional diffuse emission along a PA=214• . The origin of these two structures is unclear and deserves further investigation.

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Section: Line Identificationsupporting

confidence: 52%

Section: Origins Of the Outburst: Extinction Or Accretion?mentioning

confidence: 89%

Section: Line Identificationmentioning

confidence: 99%

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The 2008 outburst in the young stellar system Z CMa

Bonnefoy

Chauvin

Dougados

et al. 2017

A&A

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“…In these research papers, considerable speculation has been put forth as to the nature of this eruptive event, yet it is generally agreed that it is the result of a rapid and massive increase in accretion onto the surface of the young star. The reader is referred to the papers byÀbrahàm et al (2004a, 2004b, 2006), Acosta-Pulido et al (2007), Andrews et al (2004), Aspin et al (2006), Aspin et al (2008, herein ABR08), Aspin et al (2009aAspin et al ( , 2009b, Briceño et al (2004), Brittain et al (2007), Fedele et al (2007aFedele et al ( , 2007b, Gibb et al (2006), Grosso et al (2005), Kastner et al (2004Kastner et al ( , 2006, Kóspál et al (2005), Kun (2008), McGehee et al (2004), Mosoni et al (2005), Muzerolle et al (2005), Ojha et al (2005Ojha et al ( , 2006, Reipurth & Aspin (2004), Rettig et al (2005), Semkov (2004Semkov ( , 2006, Tsukagoshi et al (2005), Vacca et al (2004), Vig et al (2006), and Walter et al (2004) for further discussions.…”

Section: Introduction When the Amateur Astronomer Jay Mcneil Discovermentioning

confidence: 99%

V1647 Orionis: Optical Photometric and Spectroscopic Monitoring Through the 2003-2006 Outburst

Aspin

Reipurth

2009

The Astronomical Journal

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We present results from an optical imaging and spectroscopic monitoring campaign on the young, low-mass eruptive variable star V1647 Orionis. The star and associated nebulosity (McNeil's Nebula) were observed over the period 2004 February to 2006 February with observations commencing a few months after the original outburst event occurred. Using the Gemini North telescope, we obtained multiband optical imaging photometry and medium-resolution long-slit spectroscopy of V1647 Ori on an approximately monthly interval. During this period, V1647 Ori remained at, or close to, peak brightness and then faded by 5 mag to close to its pre-outburst brightness. This implies an outburst timescale of around 27 months. Spectral features seen in both emission and absorption varied considerably during the monitoring period. For example, the Hα line changed significantly in both intensity and profile. We present and discuss the observed photometric and spectroscopic changes and consider how this eruptive event relates to the early formative stages of low-mass stars.

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“…FUOr status was rejected by Kastner et al (2006) because the outburst didn't last long enough, and left open by Aspin et al (2006, who found only one previous outburst, in 1966-67, on a long series of plates from Harvard and Asiago). Ojha et al (2006) declared it to be an EXOr, whose prototype is not EX Ori, and Gibb et al (2006) said it was not much like either class. FU Ori itself had its disk resolved by mid-infrared interferometry during the reference year (Quanz et al 2006).…”

Section: Real-time Stellar Evolutionmentioning

confidence: 99%

Astrophysics in 2006

2007

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The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the universe) and others of which there are always many, like meteors and molecules, black holes and binaries.Comment: 244 pages, no figure

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Post‐Outburst Infrared Spectra of V1647 Ori, the Illuminating Star of McNeil’s Nebula

Cited by 21 publications

References 23 publications

The 2008 outburst in the young stellar system Z CMa

The 2008 outburst in the young stellar system Z CMa

V1647 Orionis: Optical Photometric and Spectroscopic Monitoring Through the 2003-2006 Outburst

Astrophysics in 2006

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