J/ApJS/122/221 A mid-IR survey of Proto-PNs Candidates (Meixner+, 1999)
A Mid-infrared Imaging Survey of Proto-Planetary Nebula Candidates
Meixner M., Ueta T., Dayal A., Hora J. L., Fazio G. Hrivnak B. J.,
Skinner C. J., Hoffmann W. F., Deutsch L. K.
<Astrophys. J. Suppl. Ser. 122, 221 (1999)>
=1999ApJS..122..221M 1999ApJS..122..221M
ADC_Keywords: Infrared sources; Interstellar medium; Mass loss
Keywords: circumstellar matter - infrared: ISM: continuum - ISM:
structure - stars: AGB and post-AGB - stars: mass loss
Abstract:
We present the data from a mid-infrared (MIR) imaging survey of 66
proto-planetary nebula candidates using two MIR cameras (MIRAC2 and
Berkcam) at the NASA Infrared Telescope Facility and the United
Kingdom Infrared Telescope. The goal of this survey is to determine
the size, flux, and morphology of the MIR emission regions, which
sample the inner regions of the circumstellar dust shells of
protoplanetary nebulae. We imaged these protoplanetary nebulae with
narrowband filters(δλ/λ≃10%) at wavelengths of
notable dust features. With our typical angular resolution of 1'', we
resolve 17 sources, find 48 objects unresolved, and do not detect one
source. For several sources we checked optical and infrared
associations and positions of the sources. In table format, we list
the size and flux measurements for all of the detected objects and
show figures of all of the resolved sources. The proto-planetary
nebula candidate sample includes, in addition to the predominant
proto-planetary nebulae, extreme asymptotic giant branch stars, young
planetary nebulae, a supergiant, and a luminous blue variable. We find
that dust shells that are cooler (T≃150 K) and brighter in the
infrared are more easily resolved. Eleven of the seventeen resolved
sources are extended and fall into one of two types of MIR
morphological classes: core/elliptical or toroidal. Core/elliptical
structures show unresolved cores with lower surface brightness
elliptical nebulae. Toroidal structures show limb-brightened peaks
suggesting equatorial density enhancements. We argue that
core/ellipticals have denser dust shells than toroidals.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 91 65 Characteristics of Proto-PN in mid-IR survey
table3.dat 81 186 Observed fluxes and sizes of the mid-IR survey
refs.dat 62 36 References to table1.dat
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name IRAS identification
13 A1 --- n_Name [defghijk] Note on the identification (1)
15- 17 A3 --- Chem Proto PN chemistry: C=carbon rich,
O=oxygen rich, C/O=rich in both elements
20- 29 A10 --- SType Spectral type of the central star
32- 35 F4.1 mag Vmag ? V band magnitude of the central star
37- 43 F7.2 Jy F12 IRAS Flux at 12µm
46- 52 F7.2 Jy F25 IRAS Flux at 25µm
53- 59 F7.2 Jy F60 ? IRAS Flux at 60µm
61- 66 F6.2 Jy F100 ? IRAS Flux at 100µm
70- 73 A4 --- r_MIR Comma-separated numbered references of
mid-IR spectra given in refs.dat
78- 81 F4.2 kpc Dis ? Distance the proto PN
84- 90 A7 --- r_PPN Comma-separated Lettered references
given in refs.dat (2)
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Note (1):
d = Very young PN
e = Extreme AGB star
f = RV Tauri star
g = Emission line Be star, possibly a pre-main-sequence star
h = Luminous Blue Variable
i = Supergiant j = HD 235718 (SAO 34043), a V=9.5 mag B9
star is not associated with this source. See text
k = This source is located 7''; north of IRAS coordinates. See text.
Note (2): References for other information. SIMBAD for IRAS measurements of
all sources and for V magnitudes and spectral type for many sources;
Oudmaijer et al. 1992A&AS...96..625O 1992A&AS...96..625O for V magnitudes and spectral
type of many sources. B. J. Hrivnak 1998 (private communication) for V
and spectral type of many sources
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name IRAS identification
13 A1 --- f_Name [d] Indicates the Flux, SizeS, ELS, and
PA refer to the entire shell
17- 23 A7 --- m_Name Observation date for multiple wavelength
images of an object
25- 28 F4.1 um Wave ? Wavelength of the image
30- 33 I4 Jy Flux ? Flux density of the source at Wave
36- 41 F6.2 arcsec SizeS ? Size of the source with the major axis
at the 50% contour level
43- 46 F4.2 --- ELS ? Ellipticity (1-b/a) of the source
48- 50 I3 deg PA ? Position angle
52- 55 F4.2 arcsec PSFs Size of the Point Spread Function with
the major axis at the 50% contour level
57- 60 F4.2 --- PSFe Ellipticity (1-b/a) of the Point Spread
Function
62- 64 I3 deg PSFpa Position angle of the Point Spread Function
66- 76 A11 --- Stand Standard star used
78 A1 --- f_Stand [e] Not a flux calibrator
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- Seq Sequence of references to table1.dat
6- 24 A19 --- Bibcode Reference code sequence
27- 66 A40 --- Com Comments on the references
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History:
From ApJ electronic edition
(End) Greg Schwarz (AAS) 02-Feb-2000