V2494 Cyg: a unique FU Ori type object in the Cygnus OB7 complex

Magakian, T. Yu.; Nikogossian, E. H.; Movsessian, T. A.; Моисеев, А. В.; Aspin, C.; Davis, C. J.; Pyo, Tae‐Soo; Khanzadyan, T.; Froebrich, D.; Smith, Michael D.; Moriarty‐Schieven, G. H.; Beck, Tracy

doi:10.1093/mnras/stt626

Cited by 14 publications

(11 citation statements)

References 46 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Some of the weak forbidden lines were also detected in our spectra (Figure 3) lines have been rarely observed in FUors (e.g., V2494 Cyg; Magakian et al 2013). …”

Section: Forbidden Linessupporting

confidence: 62%

The Spectroscopic Variations of the FU Orionis Object V960 Mon

Takagi

Honda

Arai

et al. 2018

View full text Add to dashboard Cite

We present the results of the spectroscopic monitoring of the FU Orionis type star V960 Mon. Spectroscopic variations of a FU Orionis type star will provide valuable information of its physical nature and the mechanism of the outburst. We conducted medium-resolution (R∼10000) spectroscopic observations of V960 Mon with 2m Nayuta telescope at the Nishi-Harima Astronomical Observatory, from 2015 January to 2017 January for 53 nights in total. We focused on Hα line and nearby atomic lines, and detected the strength variations in both absorption and emission lines. The observed variation in the equivalent width of the absorption lines correspond to a decrease in effective temperature and increase in surface gravity. These variations were likely to originate from the luminosity fading of the accretion disk due to the decrease in mass accretion rate.

show abstract

“…Some of the weak forbidden lines were also detected in our spectra (Figure 3) lines have been rarely observed in FUors (e.g., V2494 Cyg; Magakian et al 2013). …”

Section: Forbidden Linessupporting

confidence: 62%

The Spectroscopic Variations of the FU Orionis Object V960 Mon

Takagi

Honda

Arai

et al. 2018

View full text Add to dashboard Cite

show abstract

“…The presence of FUor outbursts would not be new for this region (see e.g. Rice et al 2012;Magakian et al 2013).…”

Section: Search Resultsmentioning

confidence: 99%

Extreme infrared variables from UKIDSS – I. A concentration in star-forming regions

Peña¹,

Lucas²,

Froebrich³

et al. 2014

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present initial results of the first panoramic search for high-amplitude near-infrared variability in the Galactic Plane. We analyse the widely separated two-epoch K-band photometry in the 5th and 7th data releases of the UKIDSS Galactic Plane Survey. We find 45 stars with ∆K > 1 mag, including 2 previously known OH/IR stars and a Nova. Even though the mid-plane is not yet included in the dataset, we find the majority (66%) of our sample to be within known star forming regions (SFRs), with two large concentrations in the Serpens OB2 association (11 stars) and the Cygnus-X complex (12 stars). Sources in SFRs show spectral energy distributions (SEDs) that support classification as Young Stellar Objects (YSOs). This indicates that YSOs dominate the Galactic population of high amplitude infrared variable stars at low luminosities and therefore likely dominate the total high amplitude population. Spectroscopic follow up of the DR5 sample shows at least four stars with clear characteristics of eruptive pre-main-sequence variables, two of which are deeply embedded. Our results support the recent concept of eruptive variability comprising a continuum of outburst events with different timescales and luminosities, but triggered by a similar physical mechanism involving unsteady accretion. Also, we find what appears to be one of the most variable classical Be stars.

show abstract

“…Reipurth & Aspin (1997) suggested the FUor nature of the object based on near-infrared spectra, a classification further supported by Greene et al (2008) and Aspin et al (2009b). The star brightened by R∼2.5 magnitudes sometime between 1952 and 1983 after which it seems to have reached a plateau (Magakian et al 2013). The optical spectrum shows Hα and forbidden emission lines originating from the HH 381 flow near the star, which has a projected length on the sky of 4.7 pc (Magakian et al 2013, Khanzadyan et al 2012.…”

Section: V960 Monocerotismentioning

confidence: 99%

“…The star brightened by R∼2.5 magnitudes sometime between 1952 and 1983 after which it seems to have reached a plateau (Magakian et al 2013). The optical spectrum shows Hα and forbidden emission lines originating from the HH 381 flow near the star, which has a projected length on the sky of 4.7 pc (Magakian et al 2013, Khanzadyan et al 2012. Our spectrum displays all the FUor characteristics discussed in Sect.…”

Section: V960 Monocerotismentioning

confidence: 99%

A Near-infrared Spectroscopic Survey of FU Orionis Objects

Connelley

Reipurth

2018

ApJ

138

171

View full text Add to dashboard Cite

We have conducted a homogenous near-IR spectroscopic survey of 33 objects with varying degrees of similarity to FU Orionis.Common spectroscopic features that are characteristic of the three classical FUors FU Ori, V1057 Cyg, and V1515 Cyg are: strong CO absorption, weak metal absorption, strong water bands, low gravity, strong blue shifted He I absorption, and few (if any) emission lines. Based on these criteria, we classify the 33 objects as either bona fide FUors (eruption observed), FUor-like objects (eruption not observed), or peculiar objects with some FUor-like characteristics, and present a spectral atlas of 14 bona-fide FUors, 10 FUor-like objects, and 9 peculiar objects. All objects that we classify as FUors or FUor-like have very similar near-IR spectra. We use this spectral similarity to determine the extinction to each source, and correlate the extinction to the depth of the 3 µm ice band. All bona fide FUors still today maintain the spectrum of a FUor, despite the eruption occurring up to 80 years ago. Most FUors and FUor-like objects occupy a unique space on a plot of Na+Ca vs. CO equivalent widths, whereas the peculiar objects tend to be found mostly elsewhere. Since most FUors show a reflection nebula, we also present an atlas of K-band images of each target. We found that the near-IR spectra of FUors and young brown dwarfs can be extremely similar, a distinguishing feature being the Paschen β absorption in the spectra of FUors. Although V1647 Ori, AR 6a, and V346 Normae had been previously classified as candidate FUors, we classify them as peculiar objects with some FUor-like properties since their spectra now differ significantly from bona fide FUors. We confirm two new FUor-like objects that were initially identified as candidates based on their near-IR morphology.

show abstract

V2494 Cyg: a unique FU Ori type object in the Cygnus OB7 complex

Cited by 14 publications

References 46 publications

The Spectroscopic Variations of the FU Orionis Object V960 Mon

The Spectroscopic Variations of the FU Orionis Object V960 Mon

Extreme infrared variables from UKIDSS – I. A concentration in star-forming regions

A Near-infrared Spectroscopic Survey of FU Orionis Objects

Contact Info

Product

Resources

About