Detection of a multishell planetary nebula around the hot subdwarf O-type star 2MASSJ19310888+4324577

A. Aller; L. F. Miranda; A. Ulla; R. Vázquez; P. F. Guillén; L. Olguín; C. Rodríguez-López; P. Thejll; R. Oreiro; M. Manteiga; E. Pérez

doi:10.1051/0004-6361/201219560

Detection of a multishell planetary nebula around the hot subdwarf O-type star 2MASSJ19310888+4324577

A. Aller^*, L. F. Miranda, A. Ulla, R. Vázquez, P. F. Guillén, L. Olguín, C. Rodríguez-López, P. Thejll, R. Oreiro, M. Manteiga, E. Pérez

^*Corresponding author for this work

Departamento de Investigación en Física

Research output: Contribution to journal › Article › peer-review

14 Scopus citations

Abstract

Context. The origin of hot subdwarf O-type stars (sdOs) remains unclear since their discovery in 1947. Among others, a post-asymptotic giant branch (post-AGB) origin is possible for a fraction of sdOs. Aims. We are involved in a comprehensive ongoing study to search for and to analyze planetary nebulae (PNe) around sdOs with the aim of establishing the fraction and properties of sdOs with a post-AGB origin. Methods. We used deep Hα and [Oiii] images of sdOs to detect nebular emission and intermediate-resolution, long-slit optical spectroscopy of the detected nebulae and their sdO central stars. These data were complemented with other observations (archive images, high-resolution, long-slit spectroscopy) for further analysis of the detected nebulae. Results. We report detecting an extremely faint, complex PN around 2MASSJ19310888+4324577 (2M1931+4324), a star classified as sdO in a binary system. The PN shows a bipolar and an elliptical shell, whose major axes are oriented perpendicular to each other, and high-excitation structures outside the two shells. WISE archive images show faint, extended emission at 12μm and 22μm in the inner nebular regions. The internal nebular kinematics, which is derived from high-resolution, long-slit spectra, is consistent with a bipolar and a cylindrical/ellipsoidal shell, in both cases with the main axis mainly perpendicular to the line of sight. The nebular spectrum only exhibits Hα, Hβ, and [Oiii]λλ4959,5007 emission lines, but suggests a very low-excitation ([Oiii]/Hβ ≃ 1.5), in strong contrast to the absence of low-excitation emission lines. The spectrum of 2M1931+4324 presents narrow, ionized helium absorptions that confirm the previous sdO classification and suggest an effective temperature ≥60000K. The binary nature of 2M1931+4324, its association with a complex PN and several properties of the system provide strong support for the idea that binary central stars are a crucial ingredient in the formation of complex PNe.

Original language	English
Article number	A25
Journal	Astronomy and Astrophysics
Volume	552
DOIs	https://doi.org/10.1051/0004-6361/201219560
State	Published - 2013

Bibliographical note

Funding Information:
We thank our anonymous referee for his/her comments that have been most helpful for improving the analysis and discussion of the data. We are very grateful to G. Jacoby for sharing with us the result of the binary nature of 2M1931+4324 and for useful comments. We also thank M. Tapia for fruitful comments. This paper has been supported partially by grants AYA 2009-08481, AYA 2009-14648-02, AYA 2011-30147-C03-01, and AYA 2011-30228-C03-01 of the Spanish MINECO, and by grants INCITE09 E1R312096ES, INCITE09 312191PR, and IN845B-2010/061 of Xunta de Galicia, all of them partially funded by FEDER funds. C.R.-L. has a post-doctoral contract with the JAE-Doc program “Junta para la ampliación de estudios” (CSIC) cofunded by FSE, and she acknowledges financial support by grant AYA 2010-14840 of the Spanish MINECO. R.V., L.O., and P.F.G. are supported by PAPIIT-DGAPA-UNAM grant IN109509. L.O. acknowledges support by project PROMEP/103.5/12/3590. Authors also acknowledge the staff at OAN–San Pedro Mártir (particularly to Mr. Gustavo Melgoza-Kennedy), Calar Alto, and La Palma Observatories for support during observations. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg (France), Aladin, NASA’s Astrophysics Data System Bibliographic Services, and the Spanish Virtual Observatory supported from the Spanish MEC through grant AYA2008-02156. This publication makes use of data products from (1) the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration; (2) from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation; (3) from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and other grants and contracts.

Keywords

binaries: close
planetary nebulae: individual: PNG075.9+11.6
stars: individual: 2MASS J19310888+4324577
subdwarfs

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10.1051/0004-6361/201219560

Cite this

@article{85eeef5d4d8744159629cee9f6069172,

title = "Detection of a multishell planetary nebula around the hot subdwarf O-type star 2MASSJ19310888+4324577",

abstract = "Context. The origin of hot subdwarf O-type stars (sdOs) remains unclear since their discovery in 1947. Among others, a post-asymptotic giant branch (post-AGB) origin is possible for a fraction of sdOs. Aims. We are involved in a comprehensive ongoing study to search for and to analyze planetary nebulae (PNe) around sdOs with the aim of establishing the fraction and properties of sdOs with a post-AGB origin. Methods. We used deep Hα and [Oiii] images of sdOs to detect nebular emission and intermediate-resolution, long-slit optical spectroscopy of the detected nebulae and their sdO central stars. These data were complemented with other observations (archive images, high-resolution, long-slit spectroscopy) for further analysis of the detected nebulae. Results. We report detecting an extremely faint, complex PN around 2MASSJ19310888+4324577 (2M1931+4324), a star classified as sdO in a binary system. The PN shows a bipolar and an elliptical shell, whose major axes are oriented perpendicular to each other, and high-excitation structures outside the two shells. WISE archive images show faint, extended emission at 12μm and 22μm in the inner nebular regions. The internal nebular kinematics, which is derived from high-resolution, long-slit spectra, is consistent with a bipolar and a cylindrical/ellipsoidal shell, in both cases with the main axis mainly perpendicular to the line of sight. The nebular spectrum only exhibits Hα, Hβ, and [Oiii]λλ4959,5007 emission lines, but suggests a very low-excitation ([Oiii]/Hβ ≃ 1.5), in strong contrast to the absence of low-excitation emission lines. The spectrum of 2M1931+4324 presents narrow, ionized helium absorptions that confirm the previous sdO classification and suggest an effective temperature ≥60000K. The binary nature of 2M1931+4324, its association with a complex PN and several properties of the system provide strong support for the idea that binary central stars are a crucial ingredient in the formation of complex PNe.",

keywords = "binaries: close, planetary nebulae: individual: PNG075.9+11.6, stars: individual: 2MASS J19310888+4324577, subdwarfs",

author = "A. Aller and Miranda, {L. F.} and A. Ulla and R. V{\'a}zquez and Guill{\'e}n, {P. F.} and L. Olgu{\'i}n and C. Rodr{\'i}guez-L{\'o}pez and P. Thejll and R. Oreiro and M. Manteiga and E. P{\'e}rez",

note = "Funding Information: We thank our anonymous referee for his/her comments that have been most helpful for improving the analysis and discussion of the data. We are very grateful to G. Jacoby for sharing with us the result of the binary nature of 2M1931+4324 and for useful comments. We also thank M. Tapia for fruitful comments. This paper has been supported partially by grants AYA 2009-08481, AYA 2009-14648-02, AYA 2011-30147-C03-01, and AYA 2011-30228-C03-01 of the Spanish MINECO, and by grants INCITE09 E1R312096ES, INCITE09 312191PR, and IN845B-2010/061 of Xunta de Galicia, all of them partially funded by FEDER funds. C.R.-L. has a post-doctoral contract with the JAE-Doc program “Junta para la ampliaci{\'o}n de estudios” (CSIC) cofunded by FSE, and she acknowledges financial support by grant AYA 2010-14840 of the Spanish MINECO. R.V., L.O., and P.F.G. are supported by PAPIIT-DGAPA-UNAM grant IN109509. L.O. acknowledges support by project PROMEP/103.5/12/3590. Authors also acknowledge the staff at OAN–San Pedro M{\'a}rtir (particularly to Mr. Gustavo Melgoza-Kennedy), Calar Alto, and La Palma Observatories for support during observations. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg (France), Aladin, NASA{\textquoteright}s Astrophysics Data System Bibliographic Services, and the Spanish Virtual Observatory supported from the Spanish MEC through grant AYA2008-02156. This publication makes use of data products from (1) the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration; (2) from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation; (3) from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and other grants and contracts.",

year = "2013",

doi = "10.1051/0004-6361/201219560",

language = "Ingl{\'e}s",

volume = "552",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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TY - JOUR

T1 - Detection of a multishell planetary nebula around the hot subdwarf O-type star 2MASSJ19310888+4324577

AU - Aller, A.

AU - Miranda, L. F.

AU - Ulla, A.

AU - Vázquez, R.

AU - Guillén, P. F.

AU - Olguín, L.

AU - Rodríguez-López, C.

AU - Thejll, P.

AU - Oreiro, R.

AU - Manteiga, M.

AU - Pérez, E.

N1 - Funding Information: We thank our anonymous referee for his/her comments that have been most helpful for improving the analysis and discussion of the data. We are very grateful to G. Jacoby for sharing with us the result of the binary nature of 2M1931+4324 and for useful comments. We also thank M. Tapia for fruitful comments. This paper has been supported partially by grants AYA 2009-08481, AYA 2009-14648-02, AYA 2011-30147-C03-01, and AYA 2011-30228-C03-01 of the Spanish MINECO, and by grants INCITE09 E1R312096ES, INCITE09 312191PR, and IN845B-2010/061 of Xunta de Galicia, all of them partially funded by FEDER funds. C.R.-L. has a post-doctoral contract with the JAE-Doc program “Junta para la ampliación de estudios” (CSIC) cofunded by FSE, and she acknowledges financial support by grant AYA 2010-14840 of the Spanish MINECO. R.V., L.O., and P.F.G. are supported by PAPIIT-DGAPA-UNAM grant IN109509. L.O. acknowledges support by project PROMEP/103.5/12/3590. Authors also acknowledge the staff at OAN–San Pedro Mártir (particularly to Mr. Gustavo Melgoza-Kennedy), Calar Alto, and La Palma Observatories for support during observations. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg (France), Aladin, NASA’s Astrophysics Data System Bibliographic Services, and the Spanish Virtual Observatory supported from the Spanish MEC through grant AYA2008-02156. This publication makes use of data products from (1) the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration; (2) from the 2MASS, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation; (3) from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and other grants and contracts.

PY - 2013

Y1 - 2013

N2 - Context. The origin of hot subdwarf O-type stars (sdOs) remains unclear since their discovery in 1947. Among others, a post-asymptotic giant branch (post-AGB) origin is possible for a fraction of sdOs. Aims. We are involved in a comprehensive ongoing study to search for and to analyze planetary nebulae (PNe) around sdOs with the aim of establishing the fraction and properties of sdOs with a post-AGB origin. Methods. We used deep Hα and [Oiii] images of sdOs to detect nebular emission and intermediate-resolution, long-slit optical spectroscopy of the detected nebulae and their sdO central stars. These data were complemented with other observations (archive images, high-resolution, long-slit spectroscopy) for further analysis of the detected nebulae. Results. We report detecting an extremely faint, complex PN around 2MASSJ19310888+4324577 (2M1931+4324), a star classified as sdO in a binary system. The PN shows a bipolar and an elliptical shell, whose major axes are oriented perpendicular to each other, and high-excitation structures outside the two shells. WISE archive images show faint, extended emission at 12μm and 22μm in the inner nebular regions. The internal nebular kinematics, which is derived from high-resolution, long-slit spectra, is consistent with a bipolar and a cylindrical/ellipsoidal shell, in both cases with the main axis mainly perpendicular to the line of sight. The nebular spectrum only exhibits Hα, Hβ, and [Oiii]λλ4959,5007 emission lines, but suggests a very low-excitation ([Oiii]/Hβ ≃ 1.5), in strong contrast to the absence of low-excitation emission lines. The spectrum of 2M1931+4324 presents narrow, ionized helium absorptions that confirm the previous sdO classification and suggest an effective temperature ≥60000K. The binary nature of 2M1931+4324, its association with a complex PN and several properties of the system provide strong support for the idea that binary central stars are a crucial ingredient in the formation of complex PNe.

AB - Context. The origin of hot subdwarf O-type stars (sdOs) remains unclear since their discovery in 1947. Among others, a post-asymptotic giant branch (post-AGB) origin is possible for a fraction of sdOs. Aims. We are involved in a comprehensive ongoing study to search for and to analyze planetary nebulae (PNe) around sdOs with the aim of establishing the fraction and properties of sdOs with a post-AGB origin. Methods. We used deep Hα and [Oiii] images of sdOs to detect nebular emission and intermediate-resolution, long-slit optical spectroscopy of the detected nebulae and their sdO central stars. These data were complemented with other observations (archive images, high-resolution, long-slit spectroscopy) for further analysis of the detected nebulae. Results. We report detecting an extremely faint, complex PN around 2MASSJ19310888+4324577 (2M1931+4324), a star classified as sdO in a binary system. The PN shows a bipolar and an elliptical shell, whose major axes are oriented perpendicular to each other, and high-excitation structures outside the two shells. WISE archive images show faint, extended emission at 12μm and 22μm in the inner nebular regions. The internal nebular kinematics, which is derived from high-resolution, long-slit spectra, is consistent with a bipolar and a cylindrical/ellipsoidal shell, in both cases with the main axis mainly perpendicular to the line of sight. The nebular spectrum only exhibits Hα, Hβ, and [Oiii]λλ4959,5007 emission lines, but suggests a very low-excitation ([Oiii]/Hβ ≃ 1.5), in strong contrast to the absence of low-excitation emission lines. The spectrum of 2M1931+4324 presents narrow, ionized helium absorptions that confirm the previous sdO classification and suggest an effective temperature ≥60000K. The binary nature of 2M1931+4324, its association with a complex PN and several properties of the system provide strong support for the idea that binary central stars are a crucial ingredient in the formation of complex PNe.

KW - binaries: close

KW - planetary nebulae: individual: PNG075.9+11.6

KW - stars: individual: 2MASS J19310888+4324577

KW - subdwarfs

UR - http://www.scopus.com/inward/record.url?scp=84875158820&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201219560

DO - 10.1051/0004-6361/201219560

M3 - Artículo

SN - 0004-6361

VL - 552

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A25

ER -

Detection of a multishell planetary nebula around the hot subdwarf O-type star 2MASSJ19310888+4324577

Abstract

Bibliographical note

Keywords

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