On the discovery of Comet Kohoutek (1973f)

Kohoutek, L.

doi:10.1016/0019-1035(74)90011-6

Cited by 20 publications

(25 citation statements)

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“…(1) Acker (1978), (2) Acker et al (1998), (3) , (4) Bässgen et al (1995), (5) Christianto & Seaquist (1998), (6) Ciardullo et al (1999), (7) Costero et al (1986), (8) Gathier et al (1986a), (9) Gathier et al (1986b), (10) Gurzadyan (1970) (11) Gutiérrez- Moreno et al (1999), (12) Hajian et al (1993), (13) Hajian et al (1995), (14) Hajian et al (1997), (15) Harrington & Dahn (1980), (16) Harris et al (1997), (17) Huemer & Weinberger (1988), (18) Jacoby (1988), (19) Kaler & Lutz (1985), (20) , (21) Kohoutek (1995), (22) Lutz (1973), (23) Maciel (1996), (24) Maciel & Cazetta (1997), (25) Maciel & Pottasch (1980), (26) Martin (1994), (27) Masson (1986), (28) Masson (1989), (29) Meatheringham et al (1988), (30) Mendez & Niemela (1981), (31) …”

Section: Discussionmentioning

confidence: 99%

The distance scale of planetary nebulae

Bensby

Lundström

2001

A&A

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Abstract. By collecting distances from the literature, a set of 73 planetary nebulae with mean distances of high accuracy is derived. This sample is used for recalibration of the mass-radius relationship, used by many statistical distance methods. An attempt to correct for a statistical peculiarity, where errors in the distances influences the mass-radius relationship by increasing its slope, has been made for the first time. Distances to PNe in the Galactic Bulge, derived by this new method as well as other statistical methods from the last decade, are then used for the evaluation of these methods as distance indicators. In order of achieving a Bulge sample that is free from outliers we derive new criteria for Bulge membership. These criteria are much more stringent than those used hitherto, in the sense that they also discriminate against background objects. By splitting our Bulge sample in two, one with optically thick (small) PNe and one with optically thin (large) PNe, we find that our calibration is of higher accuracy than most other calibrations. Differences between the two subsamples, we believe, are due to the incompleteness of the Bulge sample, as well as the dominance of optical diameters in the "thin" sample and radio diameters in the "thick" sample. Our final conclusion is that statistical methods give distances that are at least as accurate as the ones obtained from many individual methods. Also, the "long" distance scale of Galactic PNe is confirmed.

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Section: Discussionmentioning

confidence: 99%

The distance scale of planetary nebulae

Bensby

Lundström

2001

A&A

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“…To determine any systematic offset our data may be subject to, we compared our observed [ (1983), Kinman, Feast & Lasker (1988), Acker et al (1991), Ruffle et al (2004) and Jacoby & Van de Steene (2004) hereafter W83, KFL88, SK89, ASTR91, R04 and JaSt04, respectively, while fewer have been collated from O'Dell (1963), Kohoutek & Martin (1981), Cappellaro et al (2001), Perek (1971) and Viadana & de Freitas Pacheco (1985) hereafter O63, KM81, C01, P71 and VP85, respectively. Absolute fluxes from the literature have been measured using either photoelectric narrow-band interference filter photometry (e.g.…”

Section: Comparison With Literature Fluxesmentioning

confidence: 99%

Planetary Nebulae towards the Galactic bulge - I. [O iii] fluxes

Kovacevic

Parker

Jacoby

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present fluxes and angular diametres for 435 Planetary Nebulae (PNe) in the central 10°× 10° region towards the Galactic bulge. Our sample is taken from the new discoveries of the MASH PN surveys as well as previously known PN. This sample accounts for 80 per cent of known PN in this region. Fluxes and diametres are measured from narrow‐band imaging with the MOSAIC‐II camera on the 4‐m Blanco Telescope at the Cerro‐Tololo Inter‐American Observatory. This is the largest (∼60 deg2), uniform survey of the inner Galactic bulge ever undertaken. 104 of the objects have measured , , Hα or Hβ fluxes from the literature, which we use to undertake a detailed comparison to demonstrate the integrity of our new fluxes. Our independent measurements are in excellent agreement with the very best literature sources over two orders of magnitude, while maintaining good consistency over five orders of magnitude. The excellent resolution and sensitivity of our data allows not only for a robust set of homogenous PN fluxes, but provides greater detail into their intricate, otherwise undetermined morphologies. These new, extensive measurements significantly increase the sample of reliable fluxes for Galactic bulge PN making it a valuable resource and a prelude to the construction of our new Galactic bulge PN luminosity function (Paper II).

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“…On the night of 1996 September 3, observations were obtained of the standard stars G24-9 (five observations), GD248 (three observations) and G158-100 (two observations), all from Oke (1990), and the planetary nebulae IC 418 and NGC 6818 (four observations each), fluxes from Kohoutek & Martin (1981), in order to determine the atmospheric extinction and determine the photometric calibration. The atmospheric extinction coefficient in the [O III] λ5007 filter was found to be 0.16 ± 0.01 mag airmass −1 .…”

Section: O B S E Rvat I O N S a N D R E D U C T I O N Smentioning

confidence: 99%

Distance to NGC 253 based on the planetary nebula luminosity function

Rekola¹,

Richer²,

McCall³

et al. 2005

Monthly Notices of the Royal Astronomical Society

128

101

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We identify a sample of 14 planetary nebulae in the nearby starburst disc galaxy NGC 253, using broad‐ and narrow‐band imaging. A simple model of the stellar and dust layers in the galaxy shows that planetary nebula magnitudes are not statistically affected much by extinction. The luminosity function of the planetary nebulae is fitted with models accounting for dust, which leads to a distance to NGC 253 of μ0= 27.62+0.16−0.26 mag (d= 3.34+0.26−0.38 Mpc). This new estimate is found to be in agreement with the few existing distance estimates for this galaxy when they are all set to a common Large Magellanic Cloud distance of 18.50 mag. A weighted average of the most reliable distance estimates yields a distance of μ0= 27.7 ± 0.2 mag (d= 3.5 ± 0.2 Mpc).

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On the discovery of Comet Kohoutek (1973f)

Cited by 20 publications

References 1 publication

The distance scale of planetary nebulae

The distance scale of planetary nebulae

Planetary Nebulae towards the Galactic bulge - I. [O iii] fluxes

Distance to NGC 253 based on the planetary nebula luminosity function

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