Kinematics of Planetary Nebulae in M51's Tidal Debris

Durrell, Patrick R.; Mihos, J. Christopher; Feldmeier, John J.; Jacoby, George H.; Ciardullo, Robin

doi:10.1086/344612

Cited by 40 publications

(43 citation statements)

References 34 publications

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“…However, Durrell et al (2003) found, from a spectroscopic study of the kinematics of the planetary nebula system, that the kinematics of the northwestern tidal tails in M51 can be better explained by the single-passage models, while the receding component in the northwestern tidal tails is consistent with the results of the multiple-passage model given by Salo & Laurikainen (2000a;see their Fig. 5).…”

Section: Cluster Formation Associated With the Interaction Of Ngc 519supporting

confidence: 64%

“…In the single-passage models first introduced by Toomre & Toomre (1972), the companion galaxy NGC 5195 crossed the NGC 5194 disk in the south at a distance of 25-30 kpc about 300-500 Myr ago (Hernquist 1990;Salo & Laurikainen 2000a;Durrell et al 2003). The model uses an adopted mass ratio of NGC 5195/NGC 5194 of 1 2 to 1 3 , consistent with observations (Schweizer 1977;Smith et al 1990).…”

Section: Cluster Formation Associated With the Interaction Of Ngc 519mentioning

confidence: 85%

“…There have been numerous studies of the dynamical modeling of M51 since Toomre & Toomre's (1972) seminal paper explaining galactic bridges and tails in four interacting galaxies. To date there have been two classes of dynamical models that explain the morphological structure and dynamics of the M51 system: nearly parabolic single-passage models (e.g., Toomre & Toomre 1972) and bound multiple-passage models (Salo & Laurikainen 2000a, 2000bDurrell et al 2003).…”

Section: Cluster Formation Associated With the Interaction Of Ngc 519mentioning

confidence: 99%

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Properties of Resolved Star Clusters in M51

2005

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We present a study of compact star clusters in the nearby pair of interacting galaxies NGC 5194/5195 (M51), based on multifilter Hubble Space Telescope (HST ) WFPC2 archival images. We have detected $400 isolated, resolved clusters in five HST WFPC2 fields of the two-galaxy system. Due to our requirement that the clusters be detected based only on their morphology, which results in the selection of relatively isolated objects, we estimate that we are missing the majority (by a factor of 4-6) of clusters younger than $10 Myr due to the extreme crowding in the spiral arms and star-forming regions. Hence, we focus on the cluster population older than 10 Myr. An age distribution of the detected clusters shows a broad peak between 100 and 500 Myr, which is consistent with the crossing times of the companion galaxy NGC 5195 through the NGC 5194 disk estimated in both single-and multiple-passage dynamical models. We estimate that the peak contains $2.2-2.5 times more clusters than expected from a constant rate of cluster formation over this time interval. While there is also evidence for individual peaks near 100 and 500 Myr in the cluster age distribution (consistent with the predictions of multiple-passage models), this result requires verification. We estimate the effective radii of our sample clusters and find a median value of $3-4 pc. In addition, we see correlations of (increasing) cluster size with cluster mass (with a best-fit slope of 0:14 AE 0:03) at the $4 level, and with cluster age (0:06 AE 0:02) at the 3 level. Finally, we report for the first time the discovery of faint, extended star clusters in the companion, NGC 5195, an SB0 galaxy. These have red [(V À I ) > 1:0] colors and effective radii >7 pc, and are scattered over the disk of NGC 5195. Our results therefore indicate that NGC 5195 is currently the third known barred lenticular galaxy to have formed so-called faint fuzzy star clusters.

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Section: Cluster Formation Associated With the Interaction Of Ngc 519supporting

confidence: 64%

Section: Cluster Formation Associated With the Interaction Of Ngc 519mentioning

confidence: 85%

Section: Cluster Formation Associated With the Interaction Of Ngc 519mentioning

confidence: 99%

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Properties of Resolved Star Clusters in M51

2005

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“…The corresponding data for eight more systems from our list (object nos. 6,10,13,14,19,21,25, and 27; see Table 7 and Fig. 7 in Klimanov and Reshetnikov 2001) were taken from the LEDA and NED databases.…”

Section: Mean Parameters Of the Galaxy Samplementioning

confidence: 99%

The structure and evolution of M 51-type galaxies

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Klimanov

2003

Astron. Lett.

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We discuss the integrated kinematic parameters of 20 M 51-type binary galaxies. A comparison of the orbital masses of the galaxies with the sum of the individual masses suggests that moderately massive dark halos surround bright spiral galaxies. The relative velocities of the galaxies in binary systems were found to decrease with increasing relative luminosity of the satellite. We obtained evidence that the Tully-Fisher relation for binary members could be flatter than that for local field galaxies. An enhanced star formation rate in the binary members may be responsible for this effect. In most binary systems, the direction of orbital motion of the satellite coincides with the direction of rotation of the main galaxy. Seven candidates for distant M 51-type objects were found in the Northern and Southern Hubble Deep Fields. A comparison of this number with the statistics of nearby galaxies provides evidence for the rapid evolution of the space density of M 51-type galaxies with redshift z. We assume that M 51-type binary systems could be formed through the capture of a satellite by a massive spiral galaxy. It is also possible that the main galaxy and its satellite in some of the systems have a common cosmological origin.

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“…Fortunately, the density of these extraordinary objects is relatively low, ∼ 1 arcmin −2 per unit redshift interval brighter than 5 × 10 −17 ergs cm −2 s −1 [30]. Thus while an occasional high-redshift interloper may be found within the body of a galaxy [31], these objects are unlikely to distort the shape of the luminosity function. The second source of confusion is specific to the Virgo Cluster.…”

Section: Planetary Nebula Identificationsmentioning

confidence: 98%

Extragalactic Distances from Planetary Nebulae

Ciardullo

2003

Stellar Candles for the Extragalactic Distance Scale

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Abstract. The [O III] λ5007 planetary nebula luminosity function (PNLF) occupies an important place on the extragalactic distance ladder. Since it is the only method that is applicable to all the large galaxies of the Local Supercluster, it is uniquely useful for cross-checking results and linking the Population I and Population II distance scales. We review the physics underlying the method, demonstrate its precision, and illustrate its value by comparing its distances to distances obtained from Cepheids and the Surface Brightness Fluctuation (SBF) method. We use the Cepheid and PNLF distances to 13 galaxies to show that the metallicity dependence of the PNLF cutoff is in excellent agreement with that predicted from theory, and that no additional systematic corrections are needed for either method. However, when we compare the Cepheidcalibrated PNLF distance scale with the Cepheid-calibrated SBF distance scale, we find a significant offset: although the relative distances of both methods are in excellent agreement, the PNLF method produces results that are systematically shorter by ∼ 15%. We trace this discrepancy back to the calibration galaxies and show how a small amount of internal reddening can lead to a very large systematic error. Finally, we demonstrate how the PNLF and Cepheid distances to NGC 4258 argue for a short distance to the Large Magellanic Cloud, and a Hubble Constant that is ∼ 8% larger than that derived by the HST Key Project.

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Kinematics of Planetary Nebulae in M51's Tidal Debris

Cited by 40 publications

References 34 publications

Properties of Resolved Star Clusters in M51

Properties of Resolved Star Clusters in M51

The structure and evolution of M 51-type galaxies

Extragalactic Distances from Planetary Nebulae

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