Case of central angioma of the mandible

The LMC star, SSTISAGE1C J050756.44-703453.9, was first noticed during a survey of EROS-2 lightcurves for stars with large irregular brightness variations typical of the R Coronae Borealis (RCB) class. However, the visible spectrum showing emission lines including the Balmer and Paschen series as well as many Fe II lines is emphatically not that of an RCB star. This star has all of the characteristics of a typical UX Ori star. It has a spectral type of approximately A2 and has excited an H II region in its vicinity. However, if it is an LMC member, then it is very luminous for a Herbig Ae/Be star. It shows irregular drops in brightness of up to 2 mag, and displays the reddening and "blueing" typical of this class of stars. Its spectrum, showing a combination of emission and absorption lines, is typical of a UX Ori star that is in a decline caused by obscuration from the circumstellar dust. SSTISAGE1C J050756.44-703453.9 has a strong IR excess and significant emission is present out to 500 µm. Monte Carlo radiative transfer modeling of the SED requires that SSTISAGE1C J050756.44-703453.9 has both a dusty disk as well as a large extended diffuse envelope to fit both the mid-and far-IR dust emission. This star is a new member of the UX Ori subclass of the Herbig Ae/Be stars and only the second such star to be discovered in the LMC.

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“…It is possibly the same emission-line star (No. 129) discovered in an Hα survey by Lindsay (1963). This star also appears as No.…”

Section: Introductionmentioning

confidence: 86%

“…It is possibly the same emission-line star (No. 129) discovered in an Hα survey by Lindsay (1963). This star also appears as ) in the SAGE list of ∼1000 YSO candidates (Whitney et al 2008).…”

Section: Introductionmentioning

confidence: 99%

HERSCHELOBSERVATIONS OF A NEWLY DISCOVERED UX Ori STAR IN THE LARGE MAGELLANIC CLOUD

Clayton

Sargent

Boyer

et al. 2010

ApJ

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“…The first study was that of Henize (1956) who published the positions of 415 nebulae including 97 point-like emission sources which were considered to be PN candidates. Lindsay (1963) published 109 pointlike Hα emission sources with no continuum from a sample of about 1000 emission objects. Where emission lines other than Hα were seen, the objects were classified as PN (65 objects).…”

Section: Previous Lmc Pn Surveys: a Brief Reviewmentioning

confidence: 99%

A new population of planetary nebulae discovered in the Large Magellanic Cloud -- I. Preliminary sample

Reid¹,

Parker²

2006

Monthly Notices of the Royal Astronomical Society

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We report our initial discovery of 73 new planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) following confirmatory 2dF spectroscopy on the Anglo‐Australian Telescope. Preliminary candidate sources come from a 10 per cent sub‐area of our new deep, high‐resolution Hα map of the central 25 deg2 of the LMC obtained with the UK Schmidt Telescope. The depth of the high‐resolution map was extended to Requiv∼ 22 for Hα (4.5 × 10−17 erg cm−2 s−1Å−1) by a process of multi‐exposure median co‐addition of a dozen 2‐h Hα exposures. The resulting map is at least 1‐mag deeper than the best wide‐field narrow‐band LMC images currently available. This depth, combined with our selection technique, has also led to the discovery of extended asymptotic giant branch (AGB) haloes around many new and previously known LMC PNe for the first time. Once complete, our new survey is expected to triple the LMC PN population and have significant implications for the LMC PN luminosity function, kinematics, abundance gradients, chemical evolution and, via study of the AGB haloes, the initial to final mass relation for low‐ to intermediate‐mass stars.

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“…The catalogues of objects identified in these surveys include most classes of bright emission-line object but do not distinguish between them. Although most of the brightest objects have been studied in detail and are some of the most interesting peculiar stars known, even today many of the fainter stars have not been observed spectroscopically, so these Hα catalogues may still include some important Surveys: N,S: Henize (1956); La,b: Lindsay (1961Lindsay ( , 1963; LM: Lindsay & Mullan (1963); AL: Andrews & Lindsay (1964); BE: Bohannan & Epps (1974); MA: Meyssonnier & Azzopardi (1993). ∆λ (waveband) is in nm; D (dispersion) is inÅ/mm at Hα; m lim is the detection limit of the continuum in magnitudes; A is the survey area in sq.…”

Section: Past Surveysmentioning

confidence: 99%