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A Massive Bipolar Outflow and a Dusty Torus with Large Grains in the Preplanetary Nebula IRAS 22036+5306

Sahai, R. and Young, K. and Patel, N. A. and Sánchez Contreras, C. and Morris, M. (2006) A Massive Bipolar Outflow and a Dusty Torus with Large Grains in the Preplanetary Nebula IRAS 22036+5306. Astrophysical Journal, 653 (2). pp. 1241-1252. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20110629-113320405

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Abstract

We report high angular resolution (~1") CO J = 3-2 interferometric mapping using the Submillimeter Array (SMA) of IRAS 22036+5306 (I22036), a bipolar preplanetary nebula (PPN) with knotty jets discovered in our HST snapshot survey of young PPNs. In addition, we have obtained supporting lower resolution (~10") CO and ^(13)CO J = 1-0 observations with the Owens Valley Radio Observatory (OVRO) interferometer, as well as optical long-slit echelle spectra at the Palomar Observatory. The CO J = 3-2 observations show the presence of a very fast (~220 km s^(-1)), highly collimated, massive (0.03 M_☉) bipolar outflow with a very large scalar momentum (about 10^(39) g cm s^(-1)), and the characteristic spatiokinematic structure of bow shocks at the tips of this outflow. The Hα line shows an absorption feature blueshifted from the systemic velocity by ~100 km s-1, which most likely arises in neutral interface material between the fast outflow and the dense walls of the bipolar lobes at low latitudes. The fast outflow in I22036, as in most PPNs, cannot be driven by radiation pressure. We find an unresolved source of submillimeter (and millimeter-wave) continuum emission in I22036, implying a very substantial mass (0.02-0.04 M_☉) of large (radius gtrsim1 mm), cold (≲50 K) dust grains associated with I22036's toroidal waist. We also find that the 13C/12C ratio in I22036 is very high (0.16), close to the maximum value achieved in equilibrium CNO nucleosynthesis (0.33). The combination of the high circumstellar mass (i.e., in the extended dust shell and the torus) and the high ^(13)C/^(12)C ratio in I22036 provides strong support for this object having evolved from a massive (≳4 M_☉) progenitor in which hot-bottom-burning has occurred.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/508507DOIUNSPECIFIED
http://iopscience.iop.org/0004-637X/653/2/1241PublisherUNSPECIFIED
ORCID:
AuthorORCID
Morris, M.0000-0002-6753-2066
Additional Information:© 2006 American Astronomical Society. Received 2006 June 19; accepted 2006 August 10. We thank Nick Sterling for pointing out the importance of hot-bottom-burning in enhancing the 13C/12C ratio and Noam Soker for reading an earlier version of this paper. R. S. and M. M. thank NASA for partial financial support through an LTSA award (399.20.40.06). R. S. also thanks NASA for support from an ADP award (399.20.00.08), as well as from an STScI HST award (GO 09463.01). C. S. C.’s work was supported by the National Science Foundation through grant 9981546 to Owens Valley Radio Observatory and the Spanish MCyT under project DGES/AYA2003-2785 and the 2005 "Ramón y Cajal" program.
Funders:
Funding AgencyGrant Number
NASA Long-Term Space Astrophysics award399.20.40.06
NASA Astrophysics Data Program award399.20.00.08
Space Telescope Science Institute Hubble Space Telescope awardGO 09463.01
NSF9981546
Ministerio de Ciencia Y Tecnologia, SpainDGES/ AYA2003-2785
2005 Ramón y Cajal ProgramUNSPECIFIED
Subject Keywords:circumstellar matter; planetary nebulae: individual (IRAS 22036+5306); reflection nebulae; stars: AGB and post-AGB; stars: mass loss; stars: winds, outflows
Issue or Number:2
Record Number:CaltechAUTHORS:20110629-113320405
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20110629-113320405
Official Citation:A Massive Bipolar Outflow and a Dusty Torus with Large Grains in the Preplanetary Nebula IRAS 22036+5306 R. Sahai et al. 2006 ApJ 653 1241
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:24251
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:29 Jun 2011 19:42
Last Modified:01 Nov 2019 22:18

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