Iras 17423–1755 (Hen 3–1475) Revisited: An O-Rich High-Mass Post-Asymptotic Giant Branch Star

Manteiga, M.; García-Hernández, D. A.; Manchado, A.; García-Lario, P.

doi:10.1088/0004-6256/141/3/80

Cited by 9 publications

(8 citation statements)

References 25 publications

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“…An HST image of IRAS 17393−2727 shows a highly collimated bipolar outflow, as well as a dark lane that completely obscures the central source (Manteiga et al 2011). The infrared spectrum of this source shows bright [Ne II] nebular emission, strongly suggesting that the ionization of its central region has already started (García-Hernández et al 2007).…”

Section: Iras 17393−2727mentioning

confidence: 97%

An updated catalog of OH-maser-emitting planetary nebulae

Uscanga

Gómez

Suárez

et al. 2012

A&A

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Aims. We studied the characteristics of planetary nebulae (PNe) that show both OH maser and radio continuum emission (hereafter OHPNe). These have been proposed to be very young PNe, and therefore, they could be key objects for understanding the formation and evolution of PNe. Methods. We consulted the literature searching for interferometric observations of radio continuum and OH masers toward evolved stars, including the information from several surveys. We also processed radio continuum and OH maser observations toward PNe in the Very Large Array data archive. The high positional accuracy provided by interferometric observations allow us to confirm or reject the association between OH maser and radio continuum emission. Results. We found a total of six PNe that present both OH maser and radio continuum emissions, as confirmed with radio interferometric observations. These are bona fide OHPNe. The confirmed OHPNe present a bipolar morphology in resolved images of their ionized emission at different wavelengths, suggesting that the OH maser emission in PNe is related to nonspherical mass-loss phenomena. The OH maser spectra in PNe present a clear asymmetry, tending to show blueshifted emission with respect to the systemic velocity. Their infrared colors suggest that most of these objects are very young PNe. OHPNe do not form a homogeneous group, and seem to represent a variety of different evolutionary stages. We suggest that OH masers pumped in the asymptotic giant branch (AGB) phase may disappear during the post-AGB phase, but reappear once the source becomes a PN and its radio continuum emission is amplified by the OH molecules. Therefore, OH maser emission could last significantly longer than the previously assumed 1000 yr after the end of the AGB phase. This maser lifetime may be longer in PNe with more massive central stars, which ionize a larger amount of gas in the envelope.

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Section: Iras 17393−2727mentioning

confidence: 97%

An updated catalog of OH-maser-emitting planetary nebulae

Uscanga

Gómez

Suárez

et al. 2012

A&A

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“…4.8. IRAS 17393−2727 (OH 0.9+1.3) This source shows a bipolar morphology in the optical(Manteiga et al 2011), and its IR colors suggest that the central star is strongly obscured(Ramos-Larios et al 2012). The presence of bright [Ne II] emission indicates that it is a planetary nebula(García-Hernández et al 2007).…”

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confidence: 99%

A search for water maser emission toward obscured post-AGB star and planetary nebula candidates

Gómez

Rizzo

Suárez

et al. 2015

A&A

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Context. Water maser emission at 22 GHz is a useful probe for studying the transition between the nearly spherical mass loss in the asymptotic giant branch (AGB) to a collimated one in the post-AGB phase. In their turn, collimated jets in the post-AGB phase could determine the shape of planetary nebulae once photoionization starts. Aims. We intend to find new cases of post-AGB stars and planetary nebulae (PNe) with water maser emission, including some especially interesting and rare types: water fountains (evolved objects with high velocity collimated jets traced by water masers) or water-maser-emitting PNe. Since previous studies have shown a higher detection rate of water maser emission in evolved objects that are optically obscured, we selected a sample that contains a significant fraction of post-AGB and young PN candidate sources showing signs of strong obscuration. Methods. We searched for water maser emission in 133 evolved objects using the radio telescopes in Robledo de Chavela, Parkes, and Green Bank. Results. We detected water maser emission in 15 sources of our sample, of which seven are reported here for the first time (IRAS 13483−5905, IRAS 14249−5310, IRAS 15408−5413, IRAS 17021−3109, IRAS 17348−2906, IRAS 17393−2727, and IRAS 18361−1203. We identified three water fountain candidates: IRAS 17291−2147, with a total velocity spread of 96 km s −1 in its water maser components and two sources (IRAS 17021−3109 and IRAS 17348−2906) that show water maser emission whose velocity lies outside the velocity range covered by OH masers. We have also identified IRAS 17393−2727 as a possible new watermaser-emitting PN. Conclusions. The detection rate is higher in obscured objects (14%) than in those with optical counterparts (7%), which is consistent with previous results. Water maser emission seems to be common in objects that are bipolar in the near-IR (43% detection rate in such sources). The water maser spectra of water fountain candidates like IRAS 17291−2147 show significantly fewer maser components than others (e.g., IRAS 18113−2503). We speculate that most post-AGBs may show water maser emission with wide enough velocity spread (≥100 km s −1 ) when observed with enough sensitivity and/or for long enough periods of time. Therefore, it may be necessary to single out a special group of "water fountains", probably defined by their high maser luminosities. We also suggest that the presence of both water and OH masers in a PN is a better tracer of its youth, than is the presence of just one of these species.

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“…Smolders et al (2012) have used silicates and gehlenite to fit the observed 10 and 18µm silicate features and have also noted that grain models with a component of SiC may not fit the observed silicate features to the M-type stars. The IRAS 17423-1755 is an O-rich AGB star and it too does not fit well with grain models with SiC inclusion (see more on this AGB star in Manteiga et al (2011)).…”

Section: Discussionmentioning

confidence: 97%

“…We have also used the data from the Infrared Spectrograph IRS (Houck et al (2004)); on board the Spitzer Space Telescope, Werner et al (2004) and extracted the spectrum of four M-type and AGB stars using the Cornell Atlas of Spitzer/IRS Sources (CASSIS) extraction procedure (Lebouteiller et al (2015)). Figure 10 shows model fits with observed Spitzer data in the spectral range of 8-13µm for Mtype stars and one AGB star (see Manteiga et al (2011)). It is seen that the composite grain models or porous silicate grain models do not fit the observed Spitzer fluxes satisfactorily.…”

Section: Ir Emission From Dust and Comparison With Observed Datamentioning

confidence: 99%

Composite circumstellar dust grains

Gupta¹,

Vaidya²,

Dutta³

2016

Mon. Not. R. Astron. Soc.

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We calculate the absorption efficiencies of composite silicate grains with inclusions of graphite and silicon carbide in the spectral range 5-25µm. We study the variation in absorption profiles with volume fractions of inclusions. In particular we study the variation in the wavelength of peak absorption at 10 and 18µm. We also study the variation of the absorption of porous silicate grains. We use the absorption efficiencies to calculate the infrared flux at various dust temperatures and compare with the observed infrared emission flux from the circumstellar dust around some M-Type & AGB stars obtained from IRAS and a few stars from Spitzer satellite. We interpret the observed data in terms of the circumstellar dust grain sizes; shape; composition and dust temperature.

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Iras 17423–1755 (Hen 3–1475) Revisited: An O-Rich High-Mass Post-Asymptotic Giant Branch Star

Cited by 9 publications

References 25 publications

An updated catalog of OH-maser-emitting planetary nebulae

An updated catalog of OH-maser-emitting planetary nebulae

A search for water maser emission toward obscured post-AGB star and planetary nebula candidates

Composite circumstellar dust grains

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