Planetary Nebulae and Stellar Kinematics in the Flattened Elliptical Galaxy NGC 1344

Teodorescu, A. M.; Méndez, R. H.; Saglia, R.; Riffeser, A.; Kudritzki, Rolf‐Peter; Gerhard, Ortwin; Kleyna, Jan

doi:10.1086/497364

Cited by 37 publications

(49 citation statements)

References 32 publications

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“…If we adjust our detection rate for the difference in color, magnitude and coverage, we would have detected 224 PNe, which is similar to the 197 NGC 1344-bound objects found by Teodorescu et al (2005). We conclude that the counter-dispersed spectroscopy technique described in this paper provides an efficient strategy for collecting large PN velocity samples in the local volume and is comparable to the singly-dispersed imaging technique (Méndez et al 2001;Teodorescu et al 2005).…”

Section: The Efficiency Of the Techniquesupporting

confidence: 62%

“…The velocity of each PN can be calculated from the difference between the object's position in the narrow-band frame and the dispersed frame. This technique has also been applied to NGC 1344, another Fornax galaxy, by Teodorescu et al (2005). We compare the efficiency of those observations to ours in Sect.…”

Section: Introductionmentioning

confidence: 88%

“…As a point of comparison, Teodorescu et al (2005) applied a related technique to NGC 1344, another Fornax galaxy, using the VLT and found 197 PNe. In their technique (summarized in Méndez et al 2001), each field is imaged with broad-and narrow-band filters, and then a grism is added and the narrow-band image is dispersed.…”

Section: The Efficiency Of the Techniquementioning

confidence: 99%

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Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

McNeil

Arnaboldi

Freeman³

et al. 2010

A&A

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Aims. Using a counter-dispersed slitless spectroscopy technique, we detect and measure the line-of-sight velocities of 187 planetary nebulae (PNe) around one of the nearest cD galaxies, NGC 1399, with FORS1 on the VLT. Methods. We describe the method for identifying and classifying the emission-line sources and the procedure for computing their J2000 coordinates and velocities. The number of PN detections and the errors in the velocity measurements (37 km s −1 ) indicate that this technique is comparable to other methods. Results. We present the spatial distribution of the PNe and a basic analysis of their velocities. The PN two-dimensional velocity field shows marginal rotation consistent with other studies. We also find a low-velocity substructure in the halo and a flatter velocity-dispersion profile compared to previous observations that extends to ∼400 . The detection of a low-velocity subcomponent underscores the importance of discrete velocity tracers for the detection of un-mixed components. Conclusions. The new velocity-dispersion profile is in good agreement with revised velocity dispersions for the red globular clusters in NGC 1399. The outer parts of this profile are consistent with one of the dynamical models, which corresponds to a circular velocity of 340 km s −1 and a rescaled B-band mass-to-light ratio of 20 at 7 radius. These measurements trace the kinematics of the outer halo and disentangle the heterogenous populations in the Fornax Cluster core. The new data set the stage for a revised dynamical model of the outer halo of NGC 1399.

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Section: The Efficiency Of the Techniquesupporting

confidence: 62%

Section: Introductionmentioning

confidence: 88%

Section: The Efficiency Of the Techniquementioning

confidence: 99%

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Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

McNeil

Arnaboldi

Freeman³

et al. 2010

A&A

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“…At this distance the density is comparable to the field galaxy density (Kambas et al 2000). Sometimes classified as S0; shows rotation within 2 effective radii (Teodorescu et al 2005). NGC 2865 -isolated galaxy (Reda et al 2004), remains of a rotating HI disk (Schiminovich 1995).…”

Section: The Shell Galaxiesmentioning

confidence: 86%

Globular cluster systems of six shell galaxies

Sikkema

Peletier

Carter

et al. 2006

A&A

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Context. Shells in Elliptical Galaxies are faint, sharp-edged features, believed to provide evidence of a recent (∼0.5−2 × 10 9 years ago) merger event. We analyse the Globular Cluster (GC) systems of six shell elliptical galaxies, to examine the effects of mergers upon the GC formation history. Aims. We examine the colour distributions, and investigate differences between red and blue globular cluster populations. We present luminosity functions, spatial distributions and specific frequencies (S N ) at 50 kpc radius for our sample. Methods. We present V and I magnitudes for cluster candidates measured with the HST Advanced Camera for Surveys (ACS). Galaxy background light is modelled and removed, and magnitudes are measured in 8 pixel (0.4 arcsec) diameter apertures. Background contamination is removed using counts from Hubble Deep Field South. Results. We find that the colour distributions for NGC 3923 and NGC 5982 have a bimodal form typical of bright ellipticals, with peaks near V − I = 0.92 ± 0.04 and V − I = 1.18 ± 0.06. In NGC 7626, we find in addition a population of abnormally luminous clusters at M I = −12.5. In NGC 2865 we find an unusually blue population, which may also be young. In NGC 1344 and NGC 474 the red cluster population is marginally detected. The radial surface density profiles are more flattened than the galaxy light in the cores. As already known, in NGC 3923, which has a high S N of 5.6, the radial density distribution is more shallower than the diffuse galaxy light. Conclusions. The clusters in NGC 2865 and NGC 7626 provide evidence for formation of a population associated with a recent merger. In the other galaxies, the properties of the clusters are similar to those observed in other, non-shell, elliptical galaxies.

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“…If the PNe sample is large, obtaining the LF via the traditional χ 2 approach is relatively simple because one could fit the PNLF to a histogram built with the data (i.e., Méndez et al 2001;Teodorescu et al 2005;Johnson et al 2009). However, if the sample of PNe is small, this procedure becomes very sensitive to the parameters used to construct the histogram (i.e., bin size, number of bins, range of values used).…”

Section: Introductionmentioning

confidence: 99%

A two-mode planetary nebula luminosity function

Rodríguez-González

Hernández-Martínez

Esquivel

et al. 2015

A&A

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Context. We propose a new planetary nebula luminosity function (PNLF) that includes two populations in the distribution. Our PNLF is a direct extension of the canonical function proposed by Jacoby et al. (1987), in order to avoid problems related with the histogram construction, it is cast in terms of cumulative functions. Aims. We are interested in recovering the shape of the faint part of the PNLF in a consistent manner, for galaxies with and without a dip in their PNLFs. Methods. The parameters for the two-mode PNLF are obtained with a genetic algorithm, which obtains a best fit to the PNLF varying all of the parameters simultaneously in a broad parameter space. Results. We explore a sample of nine galaxies with various Hubble types and construct their PNLF. All of the irregular galaxies, except one, are found to be consistent with a two-mode population, while the situation is less clear for ellipticals and spirals.For the case of NGC 6822, we show that the two-mode PNLF is consistent with previous studies of the star formation history within that galaxy. Our results support two episodes of star formation, in which the second episode is significantly stronger.

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Planetary Nebulae and Stellar Kinematics in the Flattened Elliptical Galaxy NGC 1344

Cited by 37 publications

References 32 publications

Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

Counter-dispersed slitless-spectroscopy technique: planetary nebula velocities in the halo of NGC 1399

Globular cluster systems of six shell galaxies

A two-mode planetary nebula luminosity function

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