Low-dispersion spectra galactic distribution of various interesting strong- emission-line objects in the southern Milky Way.

Sanduleak, N.; Stephenson, C. B.

doi:10.1086/152464

Cited by 80 publications

(77 citation statements)

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“…From a detailed analysis of the emission lines in the high resolution optical spectrum of Hen 401 Henize (1976), Allen (1978) and Sanduleak & Stephenson (1973). The same effective temperature is needed to explain the observed strength of the nebular Balmer emission lines.…”

Section: Discussionmentioning

confidence: 99%

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IUE and ISO observations of the bipolar proto-planetary nebula Hen 401 (IRAS 10178-5958)

Parthasarathy

García-Lario

Gauba

et al. 2001

A&A

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Abstract. We present ultraviolet (IUE) and infrared (ISO) observations of the bipolar proto-planetary nebula Hen 401 which, combined with previously available optical and near infrared data, are used to reconstruct the overall spectral energy distribution from 1150Å to 100 µm. The ISO spectrum is dominated by strong PAH emission superimposed on a very cold continuum which is interpreted as thermal emission originating in the C-rich cool dust (∼106 K) present in the circumstellar envelope, the remnant of the previous AGB phase. In addition, a second, hotter component detected in the near infrared is attributed to thermal emission from hot dust (∼640 K), suggesting that mass loss and dust grain formation is still on-going during the current post-AGB phase. The ultraviolet (IUE) spectrum shows a stellar continuum in the wavelength interval 2400Å to 3200Å which corresponds to a moderately reddened B8-type central star. Unexpectedly, the UV flux in the wavelength interval 1150Å to 1900Å is very weak or absent with no evidence of a hotter binary companion which could explain the detection of the nebular emission lines observed in the available ground-based optical spectra of Hen 401. HST WFPC2 high resolution images also show no indication of a hot companion to the B8-type central star observed both in the optical and in the UV. The evolutionary implications of a possible single nature for the central star of Hen 401 are discussed.

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Section: Discussionmentioning

confidence: 99%

“…Hen 401 is an early-type emission-line star (Henize 1976;Sanduleak & Stephenson 1973) first identified as a post-asymptotic giant branch (post-AGB) star or a proto-planetary nebula (PPN) by Parthasarathy & Pottasch (1989) …”

Section: Introductionmentioning

confidence: 99%

IUE and ISO observations of the bipolar proto-planetary nebula Hen 401 (IRAS 10178-5958)

Parthasarathy

García-Lario

Gauba

et al. 2001

A&A

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“…15). Using the SIMBAD database, we identified the central star with the emission-line star Hen 3-1383, classified in the literature as an Me (The 1961;Sanduleak & Stephenson 1973;Allen 1978) or a candidate symbiotic (Henize 1976) star. Our recent optical spectroscopy of Hen 3-1383 with the Southern African Large Telescope (SALT), however, showed that the spectrum of this star is almost identical to those of the prototype LBV P Cygni (see, e.g., Stahl et al 1993) and the recently discovered candidate LBV MN 112 (Gvaramadze et al 2010b), which implies the LBV classification for Hen 3-1383 as well (Gvaramadze et al, in prep.…”

Section: Three Circular Shellsmentioning

confidence: 99%

Search for OB stars running away from young star clusters

Gvaramadze

Kniazev

Kroupa

et al. 2011

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Dynamical few-body encounters in the dense cores of young massive star clusters are responsible for the loss of a significant fraction of their massive stellar content. Some of the escaping (runaway) stars move through the ambient medium supersonically and can be revealed via detection of their bow shocks (visible in the infrared, optical or radio). In this paper, which is the second of a series of papers devoted to the search for OB stars running away from young ( < ∼ several Myr) Galactic clusters and OB associations, we present the results of the search for bow shocks around the star-forming region NGC 6357. Using the archival data of the Midcourse Space Experiment (MSX) satellite and the Spitzer Space Telescope, and the preliminary data release of the Wide-Field Infrared Survey Explorer (WISE), we discovered seven bow shocks, whose geometry is consistent with the possibility that they are generated by stars expelled from the young (∼1-2 Myr) star clusters, Pismis 24 and AH03 J1725-34.4, associated with NGC 6357. Two of the seven bow shocks are driven by the already known OB stars, HD 319881 and [N78] 34. Follow-up spectroscopy of three other bow-shockproducing stars showed that they are massive (O-type) stars as well, while the 2MASS photometry of the remaining two stars suggests that they could be B0 V stars, provided that both are located at the same distance as NGC 6357. Detection of numerous massive stars ejected from the very young clusters is consistent with the theoretical expectation that star clusters can effectively lose massive stars at the very beginning of their dynamical evolution (long before the second mechanism for production of runaway stars, based on a supernova explosion in a massive tight binary system, begins to operate) and lends strong support to the idea that probably all field OB stars have been dynamically ejected from their birth clusters. A by-product of our search for bow shocks around NGC 6357 is the detection of three circular shells typical of luminous blue variable and late WN-type Wolf-Rayet stars.

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“…A recent objective-prism survey of the southern Milky Way (Sanduleak and Stephenson 1973) has shown, as was generally anticipated, that many of the unresolved objects contained in the Catalogue of Galactic Planetary Nebulae, compiled by Perek and Kohoutek (1967), are actually strong emission-line stars of diverse types. Conversely, however, the same survey uncovered a total of only six objects that are currently cataloged as early-type emission-line stars but which are instead planetary nebulae.…”

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confidence: 73%