Radio-continuum detections of Galactic Planetary Nebulae - I. MASH PNe detected in large-scale radio surveys

Bojičić, Ivan S.; Parker, Quentin A.; Filipović, Miroslav; Frew, David J.

doi:10.1111/j.1365-2966.2010.17900.x

Cited by 28 publications

(23 citation statements)

References 61 publications

(91 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In particular, we used the list of NVSS radio continuum detections (Condon & Kaplan 1998) coincident with sources in the Strasbourg-ESO Catalog of Galactic Planetary Nebulae (Acker et al 1992), and in subsequent optical surveys (Luo et al 2005). Furthermore, we used the PNe from the the new Macquarie/AAO/Strasbourg Hα (MASH) catalog (Parker et al 2006;Miszalski et al 2008) detected at centimeter wavelengths in the NVSS and the Molonglo Galactic Plane Survey (MGPS-2; Murphy et al 2007), reported by Bojičić et al (2011). Other PNe with radio continuum observations reported elsewhere (Aaquist & Kwok 1990;Van de Steene & Pottasch 1993, 1995Van de Steene & Jacoby 2001) were also included in our list.…”

Section: Notesmentioning

confidence: 99%

An updated catalog of OH-maser-emitting planetary nebulae

Uscanga

Gómez

Suárez

et al. 2012

A&A

View full text Add to dashboard Cite

Aims. We studied the characteristics of planetary nebulae (PNe) that show both OH maser and radio continuum emission (hereafter OHPNe). These have been proposed to be very young PNe, and therefore, they could be key objects for understanding the formation and evolution of PNe. Methods. We consulted the literature searching for interferometric observations of radio continuum and OH masers toward evolved stars, including the information from several surveys. We also processed radio continuum and OH maser observations toward PNe in the Very Large Array data archive. The high positional accuracy provided by interferometric observations allow us to confirm or reject the association between OH maser and radio continuum emission. Results. We found a total of six PNe that present both OH maser and radio continuum emissions, as confirmed with radio interferometric observations. These are bona fide OHPNe. The confirmed OHPNe present a bipolar morphology in resolved images of their ionized emission at different wavelengths, suggesting that the OH maser emission in PNe is related to nonspherical mass-loss phenomena. The OH maser spectra in PNe present a clear asymmetry, tending to show blueshifted emission with respect to the systemic velocity. Their infrared colors suggest that most of these objects are very young PNe. OHPNe do not form a homogeneous group, and seem to represent a variety of different evolutionary stages. We suggest that OH masers pumped in the asymptotic giant branch (AGB) phase may disappear during the post-AGB phase, but reappear once the source becomes a PN and its radio continuum emission is amplified by the OH molecules. Therefore, OH maser emission could last significantly longer than the previously assumed 1000 yr after the end of the AGB phase. This maser lifetime may be longer in PNe with more massive central stars, which ionize a larger amount of gas in the envelope.

show abstract

Section: Notesmentioning

confidence: 99%

An updated catalog of OH-maser-emitting planetary nebulae

Uscanga

Gómez

Suárez

et al. 2012

A&A

View full text Add to dashboard Cite

show abstract

“…The small, low-excitation core is only ∼6 ′′ × 4 ′′ across, is nitrogen enriched (Vázquez et al 1998), and has an integrated flux, F (Hα) = 2.4 × 10 −13 erg cm −2 s −1 (López et al 2000). In addition, the compact core (but not the giant outflow) is detected in the radio at 6 cm (Bojičić et al 2011a). We plot the nebular core in Fig.…”

Section: A1 Backgroundmentioning

confidence: 99%

“…The extinction constants are usually determined from the Balmer decrement, as derived from optical spectroscopy, or by comparing the Balmer and radio continuum fluxes. To be as homogenous as possible, we re-calculated the radio-Hα extinctions using the radio data and methods given in Bojičić (2010) and Bojičić et al (2011aBojičić et al ( , 2011b, and references therein).…”

Section: Extinction Constantsmentioning

confidence: 99%

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

Frew¹,

Parker²,

Bojičić³

2015

Monthly Notices of the Royal Astronomical Society

Self Cite

172

127

View full text Add to dashboard Cite

Measuring the distances to Galactic planetary nebulae (PNe) has been an intractable problem for many decades. We have now established a robust optical statistical distance indicator, the Hα surface brightness -radius or S Hα -r relation, which addresses this problem. We developed this relation from a critically evaluated sample of primary calibrating PNe. The robust nature of the method results from our revised calibrating distances with significantly reduced systematic uncertainties, and the recent availability of high-quality data, including updated nebular diameters and integrated Hα fluxes. The S Hα -r technique is simple in its application, requiring only an angular size, an integrated Hα flux, and the reddening to the PN. From these quantities, an intrinsic radius is calculated, which when combined with the angular size, yields the distance directly. Furthermore, we have found that optically thick PNe tend to populate the upper bound of the trend, while optically-thin PNe fall along the lower boundary in the S Hα -r plane. This enables sub-trends to be developed which offer even better precision in the determination of distances, as good as 18 per cent in the case of optically-thin, high-excitation PNe. This is significantly better than any previous statistical indicator. We use this technique to create a catalogue of statistical distances for over 1100 Galactic PNe, the largest such compilation in the literature to date. Finally, in an appendix, we investigate both a set of transitional PNe and a range of PN mimics in the S Hα -r plane, to demonstrate its use as a diagnostic tool. Interestingly, stellar ejecta around massive stars plot on a tight locus in S Hα -r space with the potential to act as a separate distance indicator for these objects.

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

Radio-continuum detections of Galactic Planetary Nebulae - I. MASH PNe detected in large-scale radio surveys

Cited by 28 publications

References 61 publications

An updated catalog of OH-maser-emitting planetary nebulae

An updated catalog of OH-maser-emitting planetary nebulae

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

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

Contact Info

Product

Resources

About

Radio-continuum detections of Galactic Planetary Nebulae - I. MASH PNe detected in large-scale radio surveys

Cited by 28 publications

References 61 publications

An updated catalog of OH-maser-emitting planetary nebulae

An updated catalog of OH-maser-emitting planetary nebulae

The H surface brightness-radius relation: a robust statistical distance indicator for planetary nebulae

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

Contact Info

Product

Resources

About

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