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

Parthasarathy, M.; García-Lario, P.; Gauba, G.; Martino, D. de; Nakada, Y.; Fujii, Takeshi; Pottasch, [No Value]; Cordoba, Lsf de

doi:10.1051/0004-6361:20010964

Cited by 9 publications

(13 citation statements)

References 30 publications

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“…In addition to the cold dust, warm dust indicative of recent or ongoing post-AGB mass loss may also be present in the circumstellar envelopes of these stars (e.g. Hen401, Parthasarathy et al 2001). Young massive OB supergiants are not expected at high galactic latitudes.…”

Section: Target Selectionmentioning

confidence: 99%

Photometry and low resolution spectroscopy of hot post-AGB candidates

Gauba

Parthasarathy

Kumar³

et al. 2003

A&A

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Abstract.We have obtained Johnson U, B, V and Cousins R, I photometry and low resolution spectra of a small sample of hot post-AGB candidates. Using the present data in combination with JHK data from 2MASS, infrared data from the MSX catalog and the IRAS fluxes, we have studied the spectral energy distribution (SED) of these stars. Using the DUSTY code we have estimated the dust temperatures, the distances to the stars, the mass-loss rates, angular radii of the inner boundary of the dust envelopes and dynamical ages from the tip of the AGB. These candidates have also been imaged through a narrow band Hα filter, to search for nebulosity around the central stars. Our Hα images revealed the bipolar morphology of the low excitation PN IRAS 17395-0841 with an angular extent of 2.8 . The bipolar lobes of IRAS 17423-1755 in Hα were found to have an angular extent of 3.5 (south-east lobe) and 2.2 (north-west lobe). The dust envelope characteristics, low resolution spectrum and IRAS colors suggest that IRAS 18313-1738 is similar to the proto-planetary nebula (PPN) HD 51585. The SED of IRAS 17423-1755, IRAS 18313-1738 and IRAS 19127+1717 show a warm dust component (in addition to the cold dust) which may be due to recent and ongoing mass-loss.

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Section: Target Selectionmentioning

confidence: 99%

Photometry and low resolution spectroscopy of hot post-AGB candidates

Gauba

Parthasarathy

Kumar³

et al. 2003

A&A

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“…The most important one is that the Hα line clearly presents a double peak rather than the P-Cygni profile proposed by Parthasarathy et al (2001) on the basis of low-resolution data. As can be seen in Fig.…”

Section: High Resolutionmentioning

confidence: 86%

“…M 2-9) is due to mass outflows. Indeed, Parthasarathy et al (2001) suggests that the asymmetry in Hα seen in SS73 21 is probably due to a P-Cygni profile. However, as presented in Sect.…”

Section: The Nature Of Rjha 49 and Ss73 21mentioning

confidence: 99%

Spectroscopic analysis of two peculiar emission-line stars: RJHA 49 and SS73 21

Pereira

Marcolino

Machado

et al. 2007

A&A

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Aims. We investigate the spectra and the evolutionary stages of two peculiar emission-line stars: RJHA 49 and SS73 21. Methods. We used low and high resolution optical data. Line identifications and measurements were performed for several features in their spectra.Results. For each object, we derived the extinction and the excitation temperature from a set of [Fe ii] lines and the electron density from [N ii] lines. For RJHA 49, no detailed spectroscopic study has been done so far. Our low resolution spectrum have confirmed the main characteristics found in previous works on SS73 21. On the other hand, from our high resolution data, we find that the Hα line presents a double peak, in contrast with the suggestion in the literature that it should reveal a P-Cygni profile. Surprisingly, we found a few He i transitions resembling P-Cygni profiles (e.g. He i λ5876), directly suggesting that mass loss is active in SS73 21. We also discuss the nature of these two objects based on data obtained. Although the evolutionary status of SS73 21 seems well established from previous studies (a proto-planetary nebula), the situation for RJHA 49 is not very clear mainly due to its unknown distance.However, from the strength of [N ii] λ5754 relative to [O i] λ6300, the possibility of RJHA 49 being a LBV object is reduced, and a B[e]-supergiant or a proto-planetary nebula status is more plausible.

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“…The optical spectra of these two stars show several emission lines and low excitation nebular emission lines, indicating the presence of B-type central stars (Riera et al 2003;Garcia-Lario et al 1999). In the case of Hen 3-401, the UV spectrum shows a stellar continuum in the wavelength interval 2400Å to 3200Å, which corresponds to a moderately reddened B8 type central star (Parthasarathy et al 2001a). Sahai et al (1999) from HST high resolution images find two very long bipolar outflow lobes.…”

Section: Hot Post-agb Starsmentioning

confidence: 98%