Challenges of Using Planetary Nebulae for Extragalactic Distances

Bottinelli, L.; Gouguenheim, L.; Paturel, G.; Teerikorpi, P.

doi:10.1007/978-94-010-9374-3_92

Cited by 92 publications

(175 citation statements)

References 7 publications

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“…Our new linewidth measurements are in good agreement with the Jodrell Bank measurements of StaveleySmith & Davies (1988) and measurements we performed from new HIPASS data (see Barnes et al, in prep. for a description of HIPASS), but are lower than the values published by Bottinelli et al (1982). No published H i observations are available for UGC 3141.…”

Section: Comparison Of New Hi Data With Previous Measurements and Commentioning

confidence: 67%

H i observations of giant low surface brightness galaxies

Matthews

Driel

Monnier-Ragaigne

2001

A&A

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Abstract. We have used the Nançay Radio Telescope to obtain new global H i data for 16 giant low surface brightness (LSB) galaxies. Our targets have optical luminosities and disk scale lengths at the high end for spiral galaxies (L B ∼ 10 10 L and h r ∼ >6 kpc for H 0 =75 km s −1 Mpc −1 ), but they have diffuse stellar disks, with mean disk surface brightnesses ∼ >1 magnitude fainter than normal giant spirals. Thirteen of the galaxies previously had been detected in H i by other workers, but the published H i observations were either confused, resolved by the telescope beam, of low signal-to-noise, or showed significant discrepancies between different authors. For the other 3 galaxies, no H i data were previously available. Several of the galaxies were resolved by the Nançay 3 .6 E-W beam, so global parameters were derived from multiple-point mapping observations. Typical H i masses for our sample are ∼ > 10 10 M , with M HI /L B =0.3-1.7 (in solar units). All of the observed galaxies have published optical surface photometry, and we have compiled key optical measurements for these objects from the literature. We frequently find significant variations among physical parameters of giant LSB galaxies reported by various workers.

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Section: Comparison Of New Hi Data With Previous Measurements and Commentioning

confidence: 67%

H i observations of giant low surface brightness galaxies

Matthews

Driel

Monnier-Ragaigne

2001

A&A

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“…That underestimated value would lead to pushing the galaxy out of the TF relation. The galaxy has a B-band internal extinction of 0.41 (determined using Bottinelli et al 1995). To lie on the 1σ relation, this galaxy should have an internal extinction of ∼1.3 mag, which is a very unlikely value.…”

Section: Fig 4 B-bandmentioning

confidence: 99%

“…These differences are consistent with the errors of 0.7 and 0.5 mag given in Hickson et al (1989), for both galaxies. The B T magnitudes were then corrected by Galactic extinction (Schlegel et al 1998) and by the extinction due to the inclination (Bottinelli et al 1995). Values for the galactic extinction and extinction due to the inclination were taken directly from HyperLeda.…”

Section: Magnitudesmentioning

confidence: 99%

Kinematics of galaxies in compact groups

Torres-Flores

Oliveira²,

Amram

et al. 2010

A&A

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We obtained new Fabry-Perot data cubes and derived velocity fields, monochromatic, and velocity dispersion maps for 28 galaxies in the Hickson compact groups 37, 40, 47, 49, 54, 56, 68, 79, and 93. We also derived rotation curves for 9 of the studied galaxies, 6 of which are strongly asymmetric. Combining these new data with previously published 2D kinematic maps of compact group galaxies, we investigated the differences between the kinematic and morphological position angles for a sample of 46 galaxies. We find that one third of the unbarred compact group galaxies have position angle misalignments between the stellar and gaseous components. This and the asymmetric rotation curves are clear signatures of kinematic perturbations, probably because of interactions among compact group galaxies. A comparison between the B-band Tully-Fisher relation for compact group galaxies and for the GHASP field-galaxy sample shows that, despite the high fraction of compact group galaxies with asymmetric rotation curves, these lay on the TF relation defined by galaxies in less dense environments, although with more scatter. This agrees with previous results, but now confirmed for a larger sample of 41 galaxies. We confirm the tendency for compact group galaxies at the low-mass end of the Tully-Fisher relation (HCG 49b, 89d, 96c, 96d, and 100c) to have either a magnitude that is too bright for its mass (suggesting brightening by star formation) and/or a low maximum rotational velocity for its luminosity (suggesting tidal stripping). These galaxies are outside the Tully Fisher relation at the 1σ level, even when the minimum acceptable values of inclinations are used to compute their maximum velocities. Including such galaxies with v < 100 km s −1 in the determination of the zero point and slope of the compact group B-band Tully-Fisher relation would strongly change the fit, making it different from the relation for field galaxies, which has to be kept in mind when studying scaling relations of interacting galaxies, especially at high redshifts.

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“…infall (Bottinelli et al 1986;Sandage & Tammann 1990) and assuming H 0 = 75 km s À1 Mpc À1 , LEDA also lists a kinematic distance of D = 10.09 Mpc. Finally, although relatively isolated, NGC 3184 is cataloged to be in a small group of four galaxies (Tully 1988), two of which have had Cepheid distances derived by the HST Key Project (see Freedman et al 2001 and references therein).…”

Section: Epm Distancementioning

confidence: 99%

A Study of the Type II-Plateau Supernova 1999[CLC]gi[/CLC] and the Distance to its Host Galaxy, NGC 3184

Leonard

Filippenko

et al. 2002

The Astronomical Journal

151

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We present optical spectra and photometry sampling the first 6 months after discovery of supernova (SN) 1999gi in NGC 3184. SN 1999gi is shown to be a Type II-plateau event with a photometric plateau lasting until about 100 days after discovery. Using the expanding photosphere method (EPM), we derive a distance to SN 1999gi of 11:1 þ2:0 À1:8 Mpc and an explosion date of 1999 December 5:8 þ3:0 À3:1 , or 4:1 þ3:0 À3:1 days prior to discovery. This distance is consistent with a Tully-Fisher distance recently derived to NGC 3184 (D % 11.59 Mpc), but it is somewhat closer than the Cepheid distances recently derived to two galaxies that have generally been assumed to be associated with the group containing NGC 3184 (NGC 3319, D = 13.30 AE 0.55 Mpc, and NGC 3198, D = 13.80 AE 0.51 Mpc). From many lines of evidence, we conclude that SN 1999gi is only minimally reddened. A comparison between the color of SN 1999gi at early times and that of an infinitely hot blackbody restricts the reddening to E(BÀV ) < 0.45 mag, while a comparison between the color evolution of SN 1999gi and the well-observed (and extensively modeled) Type II-P SN 1999em implies an even more restrictive upper reddening limit of E(BÀV ) < 0.3 mag. A variety of other, independent reddening estimates are consistent with these upper limits and yield a probable reddening of E(BÀV ) = 0.21 AE 0.09 mag. We reconsider the upper mass limit (9 þ3 À2 M ) recently placed on the progenitor star of SN 1999gi by Smartt et al. in light of these results. Following the same procedures, but using the new data presented here, we arrive at a less restrictive upper mass limit of 15 þ5 À3 M for the progenitor. The increased upper limit results mainly from the larger distance derived through the EPM than was assumed by the Smartt et al. analyses, which relied on less precise (and less recent) distance measurements to NGC 3184. Finally, we confirm the existence of '' complicated '' P Cygni line profiles in early-time and later photospheric-phase spectra of SN 1999gi. These features, first identified by Baron et al. in spectra of SN 1999em as high-velocity absorptions, in addition to the '' normal '' lower velocity component, are here verified to be true P Cygni profiles consisting of both an absorption trough and an emission peak at early times. In the earliest spectrum, taken less than a day after discovery, the features extend out to nearly À30,000 km s À1 , indicating the existence of very high velocity material in the outer envelope of SN 1999gi.

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Challenges of Using Planetary Nebulae for Extragalactic Distances

Cited by 92 publications

References 7 publications

H i observations of giant low surface brightness galaxies

H i observations of giant low surface brightness galaxies

Kinematics of galaxies in compact groups

A Study of the Type II-Plateau Supernova 1999[CLC]gi[/CLC] and the Distance to its Host Galaxy, NGC 3184

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