Version 2000 of the Catalogue of Galactic Planetary Nebulae

Kohoutek, L.

doi:10.1051/0004-6361:20011162

Cited by 105 publications

(108 citation statements)

References 8 publications

(4 reference statements)

Supporting

Mentioning

102

Contrasting

Unclassified

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“…Therefore these observations resolve the previous uncertainty about the nature of K 3-22: the source was included in the list of true or probable planetary nebulae (PNe) in the Strasbourg-ESO catalogue but with the note "possibly an H ii region" (Acker et al 1992), classified as a possible planetary nebula (Kohoutek 2001), or considered as an object of uncertain nature (Acker et al 1987). …”

Section: A Symbiotic Star's Spectrummentioning

confidence: 81%

K 3–22: a D-type symbiotic star

Corradi

Giammanco

2010

A&A

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A goal of the IPHAS survey is to determine the frequency and nature of emission-line sources in the Galactic plane. According to our selection criteria, K 3-22 is a candidate symbiotic star, but it was previously classified as a planetary nebula. To determine its nature, we acquired a low-resolution optical spectrum of K 3-22. Our analysis of our spectroscopy demonstrates that K 3-22 is indeed a D-type symbiotic star, because of its high excitation nebular spectrum and the simultaneous presence of Raman-scattered O vi emission at 6825 Å and 7082 Å, which is detected primarily in symbiotic stars.

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Section: A Symbiotic Star's Spectrummentioning

confidence: 81%

K 3–22: a D-type symbiotic star

Corradi

Giammanco

2010

A&A

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“…Sample from Kohoutek (2001). For some sources (IRAS 04296+3429, IRAS 04395+3601, IRAS 05113+1347, IRAS 05341+0852, IRAS 05381 +1012) the coordinates listed here are slightly different than those reported in Kohoutek (2001). In these cases, the coordinates are within ∼1″ from Simbad coordinates (Zacharias et al 2003).…”

Section: Low-mass Star-forming Regions and Evolved Starsmentioning

confidence: 89%

“…Most of these sources have been classified as Class 0 and/or Class I, which means that they harbor a protostar that is accreting material and which is bright in the mid-infrared or at least the far-infrared wavelength range. The oxygen-rich late type stars were selected from Benson et al (1990); carbon stars were selected from Alksnis et al (2001); PN and post-AGB sources are from Kohoutek (2001).…”

Section: Low-mass Star-forming Regions and Evolved Starsmentioning

confidence: 99%

Formaldehyde Masers: Exclusive Tracers of High-Mass Star Formation

Araya

Olmi

Ortiz

et al. 2015

ApJS

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The detection of four formaldehyde (H 2 CO) maser regions toward young high-mass stellar objects in the last decade, in addition to the three previously known regions, calls for an investigation of whether H 2 CO masers are an exclusive tracer of young high-mass stellar objects. We report the first survey specifically focused on the search for 6 cm H 2 CO masers toward non high-mass star-forming regions (non HMSFRs). The observations were conducted with the 305 m Arecibo Telescope toward 25 low-mass star-forming regions, 15 planetary nebulae and post-AGB stars, and 31 late-type stars. We detected no H 2 CO emission in our sample of non HMSFRs. To check for the association between high-mass star formation and H 2 CO masers, we also conducted a survey toward 22 high-mass star-forming regions from a Hi-GAL (Herschel infrared Galactic Plane Survey) sample known to harbor 6.7 GHz CH 3 OH masers. We detected a new 6 cm H 2 CO emission line in G32.74−0.07. This work provides further evidence that supports an exclusive association between H 2 CO masers and young regions of high-mass star formation. Furthermore, we detected H 2 CO absorption toward all Hi-GAL sources, and toward 24 low-mass starforming regions. We also conducted a simultaneous survey for OH (4660, 4750, 4765 MHz), H110α (4874 MHz), HCOOH (4916 MHz), CH 3 OH (5005 MHz), and CH 2 NH (5289 MHz) toward 68 of the sources in our sample of non HMSFRs. With the exception of the detection of a 4765 MHz OH line toward a pre-planetary nebula (IRAS 04395+3601), we detected no other spectral line to an upper limit of 15 mJy for most sources.

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“…This sequence is similar to the order of FWZPs (Figure 11 Acker et al (1992) classified this source as a possible PN, which is a faint object highly reddened showing a weak H-alpha emission. Kohoutek (2001) and Bojičić et al (2011) also designated this source as PN in an extensive radio-continuum survey. However, the possibility of being a PN seems to be low because the SiO maser emission is not detected from a PN.…”

Section: Maser and Infrared Properties Associated With A Post-agb Stamentioning

confidence: 99%

MONITORING OBSERVATIONS OF H₂O AND SiO MASERS TOWARD POST-AGB STARS

Kim¹,

Cho²,

Yoon³

2016

Journal of The Korean Astronomical Society

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We present the results of simultaneous monitoring observations of H 2 O 6 1,6 -5 2,3 (22 GHz) and SiO J=1-0, 2-1, 3-2 maser lines (43, 86, 129 GHz) toward five post-AGB (candidate) stars, using the 21-m single-dish telescopes of the Korean VLBI Network. Depending on the target objects, 7 -11 epochs of data were obtained. We detected both H 2 O and SiO maser lines from four sources: OH16.1−0.3, OH38.10−0.13, OH65.5+1.3, and IRAS 19312+1950. We could not detect H 2 O maser emission toward OH13.1+5.1 between the late OH/IR and post-AGB stage. The detected H 2 O masers show typical doublepeaked line profiles. The SiO masers from four sources, except IRAS 19312+1950, show the peaks around the stellar velocity as a single peak, whereas the SiO masers from IRAS 19312+1950 occur above the red peak of the H 2 O maser. We analyzed the properties of detected maser lines, and investigated their evolutionary state through comparison with the full widths at zero power. The distribution of observed target sources was also investigated in the IRAS two-color diagram in relation with the evolutionary stage of post-AGB stars. From our analyses, the evolutionary sequence of observed sources is suggested as OH65.5+1.3 → OH13.1+5.1 → OH16.1−0.3 → OH38.10−0.13, except for IRAS 19312+1950. In addition, OH13.1+5.1 from which the H 2 O maser has not been detected is suggested to be on the gateway toward the post-AGB stage. With respect to the enigmatic object, IRAS 19312+1950, we could not clearly figure out its nature. To properly explain the unusual phenomena of SiO and H 2 O masers, it is essential to establish the relative locations and spatial distributions of two masers using VLBI technique. We also include the 1.2 -160 µm spectral energy distribution using photometric data from the following surveys: 2MASS, W ISE, M SX, IRAS, and AKARI (IRC and FIS). In addition, from the IRAS LRS spectra, we found that the depth of silicate absorption features shows significant variations depending on the evolutionary sequence, associated with the termination of AGB phase mass-loss.

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Version 2000 of the Catalogue of Galactic Planetary Nebulae

Cited by 105 publications

References 8 publications

K 3–22: a D-type symbiotic star

K 3–22: a D-type symbiotic star

Formaldehyde Masers: Exclusive Tracers of High-Mass Star Formation

MONITORING OBSERVATIONS OF H₂O AND SiO MASERS TOWARD POST-AGB STARS

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Version 2000 of the Catalogue of Galactic Planetary Nebulae

Cited by 105 publications

References 8 publications

K 3–22: a D-type symbiotic star

K 3–22: a D-type symbiotic star

Formaldehyde Masers: Exclusive Tracers of High-Mass Star Formation

MONITORING OBSERVATIONS OF H2O AND SiO MASERS TOWARD POST-AGB STARS

Contact Info

Product

Resources

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MONITORING OBSERVATIONS OF H₂O AND SiO MASERS TOWARD POST-AGB STARS