A pilot study of the radio‐continuum emission from MASH planetary nebulae

Bojičić, Ivan S.; Parker, Quentin A.; Frew, David J.; Vaughan, A. E.; Filipović, Miroslav; Gunawardhana, Madusha

doi:10.1002/asna.201011571

“…A comparable mean value is derived for filled elliptical bubbles, in the hypothesis that they are PNe, and for PNe in Ingallinera et al (2014b). Similar values are found by Bojičić et al (2011) in their study of the radio emission of 26 PNe from the Macquarie/AAO/Strasbourg Hα (MASH) catalogue . A PN with a diameter of 0.4 pc is seen under an angle of 12 arcsec if it is located at about 6.9 kpc from the observer.…”

Section: Completeness Of the Bubbles Catalogue With Respect To Planetsupporting

confidence: 86%

High-resolution Very Large Array observations of 18 MIPSGAL bubbles

Ingallinera¹,

Trigilio²,

Leto³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present radio observations of 18 MIPSGAL bubbles performed at 5 GHz (6 cm) with the Karl G. Jansky Very Large Array in configuration B and BnA. The observations were aimed at understanding what kind of information high-resolution and high-sensitivity radio maps can supply on the circumstellar envelopes of different kinds of evolved stars and what their comparison with infrared images with similar resolution can tell us. We found that the 18 bubbles can be grouped into five categories according to their radio morphology. The three bubbles presenting a central point source in the radio images all correspond to luminous blue variable star candidates. Eleven bubbles show an elliptical shape and the total lack of a central object in the radio, and are likely associated with planetary nebulae. Under this assumption we derive their distance, their ionized mass and their distribution on the Galactic plane. We discuss the possibility that the MIPSGAL bubbles catalogue (428 objects) may contain a large fraction of all Galactic planetary nebulae located at a distance between 1.4 kpc and 6.9 kpc and lying in the MIPSGAL field of view. Among the remaining bubbles we identify also a H II region and a proto-planetary nebula candidate.

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“…The distances given in Table 13 supersede any SHα-r distances previously published (Pierce et al 2004;Frew et al 2006bFrew et al , 2011F08;Viironen et al 2009Viironen et al , 2011Bojičić et al 2011b;Corradi et al 2011) using earlier calibrations of the SHα-r relation, though in all cases the differences in distances are less than five per cent.…”

Section: The Distance Cataloguesupporting

confidence: 69%

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

Frew,

Parker,

Bojicic

2015

Preprint

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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.

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“…The distances given in Table 13 supersede any SHα-r distances previously published (Pierce et al 2004;Frew et al 2006bFrew et al , 2011F08;Viironen et al 2009Viironen et al , 2011Bojičić et al 2011b;Corradi et al 2011) using earlier calibrations of the SHα-r relation, though in all cases the differences in distances are less than five per cent.…”

Section: The Distance Cataloguesupporting

confidence: 68%

“…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

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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.

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A pilot study of the radio‐continuum emission from MASH planetary nebulae

Cited by 9 publications

References 45 publications

High-resolution Very Large Array observations of 18 MIPSGAL bubbles

High-resolution Very Large Array observations of 18 MIPSGAL bubbles

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

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

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