A dataset provided by the European Space Agency

Name OT1_hdinerst_1
Title How Cool Are Planetary Nebulae?
URL

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DOI https://doi.org/10.5270/esa-es6krlz
Author dinerstein, h.
Description We propose to observe the O III 52 and 88 micron fine-structure lines
with PACS in planetary nebulae, in order to investigate whether
they contain a cold and possibly metal-rich component in addition to the
ordinary hot (10,000 K) material. The presence of cold gas has been
proposed in order to account for the excessive strengths of optical
emission lines from recombining O++ ions, and low temperatures (500 -
5000 K) indicated by some diagnostics. If planetary nebulae truly have such
inhomogeneous physical conditions and abundances, this calls into
question our fundamental understanding of the composition of the nebular
gas, a major source of recycled material to the ISM. The FIR O III
lines offer a unique opportunity to address this issue because, due to
their low excitation energies, they are emitted from both cold and hot
gas, while the optical O III lines arise only from hot gas. The bright 52 and
88 micron lines were easily observed in some of our sample using less
sensitive, large-beam instruments such as the Kuiper Airborne
Observatory (by this P.I.) and ISO-LWS. For several targets the
previous observations indicate O/H values greater than solar, supporting
the idea that metal-rich gas is present, but the higher angular
resolution of PACS is needed in order to discern whether the metal-rich
material is concentrated towards the central regions, as claimed by
optical studies. For several objects we propose to also measure the 88.8
micron 1312 H I line, which will not only provide a
measurement of H+, but also a probe of temperature by
comparing its strength to that of shorter-wavelength H I lines. The
latter will be taken from Spitzer-IRS maps (for a few targets),
and optical integrated-field unit spectral maps either already obtained,
or to be obtained, at McDonald Observatory. These observations may
enable us to prove or disprove the presence of cold O-rich material in
planetary nebulae.
Publication
  • THROES: a caTalogue of HeRschel Observations of Evolved Stars. I. PACS range spectroscopy | Ramos-Medina J. et al. | Astronomy & Astrophysics Volume 611 id.A41 38 pp. | 611 | 10.1051\\/0004-6361\\/201731940 | 2018A&A...611A..41R | http://adsabs.harvard.edu/abs/2018A%26A...611A..41R
Instrument PACS_PacsRangeSpec_point, PACS_PacsLineSpec_point
Temporal Coverage 2011-05-12T22:36:23Z/2012-09-12T08:45:36Z
Version SPG v14.2.0
Mission Description Herschel was launched on 14 May 2009! It is the fourth cornerstone mission in the ESA science programme. With a 3.5 m Cassegrain telescope it is the largest space telescope ever launched. It is performing photometry and spectroscopy in approximately the 55-671 µm range, bridging the gap between earlier infrared space missions and groundbased facilities.
Creator Contact https://support.cosmos.esa.int/h®erschel/
Date Published 2013-03-12T06:06:57Z
Keywords Herschel, HSC, submillimetre, far-infrared, HIFI, PACS, SPIRE
Publisher And Registrant European Space Agency
Credit Guidelines European Space Agency, dinerstein et al., 2013, 'How Cool Are Planetary Nebulae?', SPG v14.2.0, European Space Agency, https://doi.org/10.5270/esa-es6krlz