A search for box- or peanut-shaped bulges

Jarvis, B. J.

doi:10.1086/113980

Cited by 69 publications

(66 citation statements)

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“…It is very close to exactly edge-on and its dust lane can be traced to the edges of the galaxy. Conspicuous properties of this galaxy are its box-or peanut-shaped bulge (Kormendy & Illingworth 1982;Jarvis 1986;García-Burillo et al 1999) and the warp in the gas and stellar distribution (2007) and Xilouris et al (1999). The panels on the right-hand side show the residual images corresponding to these models.…”

Section: Application On Observed Data: Ngc 4013mentioning

confidence: 99%

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

Geyter

Baes

Fritz

et al. 2013

A&A

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We present FitSKIRT, a method to efficiently fit radiative transfer models to UV/optical images of dusty galaxies. These images have the advantage that they have better spatial resolution compared to FIR/submm data. FitSKIRT uses the GAlib genetic algorithm library to optimize the output of the SKIRT Monte Carlo radiative transfer code. Genetic algorithms prove to be a valuable tool in handling the multi-dimensional search space as well as the noise induced by the random nature of the Monte Carlo radiative transfer code. FitSKIRT is tested on artificial images of a simulated edge-on spiral galaxy, where we gradually increase the number of fitted parameters. We find that we can recover all model parameters, even if all 11 model parameters are left unconstrained. Finally, we apply the FitSKIRT code to a V-band image of the edge-on spiral galaxy NGC 4013. This galaxy has been modeled previously by other authors using different combinations of radiative transfer codes and optimization methods. Given the different models and techniques and the complexity and degeneracies in the parameter space, we find reasonable agreement between the different models. We conclude that the FitSKIRT method allows comparison between different models and geometries in a quantitative manner and minimizes the need of human intervention and biasing. The high level of automation makes it an ideal tool to use on larger sets of observed data.

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Section: Application On Observed Data: Ngc 4013mentioning

confidence: 99%

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

Geyter

Baes

Fritz

et al. 2013

A&A

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“…5. It is classified either as an Sb or as an Sc type galaxy showing Hii regions, and it is characterised by a conspicuous peanut-shaped or boxy bulge (Jarvis 1986;de Souza & Dos Anjos 1987). With a fitted inclination of 89.…”

Section: Ic 2531mentioning

confidence: 99%

“…2, is variously classified as an Sbc (Xilouris et al 1999), an Sb or an SAb type galaxy with Hii regions and is considered a LINER galaxy. Furthermore, the galaxy possesses a box-shaped bulge (Jarvis 1986;de Souza & Dos Anjos 1987) and shows a very clear warp in various bands but sometimes in opposite directions for the dust, gas and stellar component of the galaxy disc (Bottema et al 1987;Sanchez-Saavedra et al 1990;Florido et al 1991;Bottema 1995Bottema , 1996, although Xilouris et al (1999) claim the stellar distribution in their optical images has no warp significant enough to affect their model. The inclination angle estimates for this galaxy vary from 89.…”

Section: Ngc 4013mentioning

confidence: 99%

HERschelObservations of Edge-on Spirals (HEROES)

Verstappen

Fritz

Baes

et al. 2013

A&A

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Context. Edge-on spiral galaxies with prominent dust lanes provide us with an excellent opportunity to study the distribution and properties of the dust within them. The HEROES project was set up to observe a sample of seven large edge-on galaxies across various wavelengths for this investigation. Aims. Within this first paper, we present the Herschel observations and perform a qualitative and quantitative analysis on them, and we derive some global properties of the far infrared and submillimetre emission. Methods. We determine horizontal and vertical profiles from the Herschel observations of the galaxies in the sample and describe the morphology. Modified black-body fits to the global fluxes, measured using aperture photometry, result in dust temperatures and dust masses. The latter values are compared to those that are derived from radiative transfer models taken from the literature. Results. On the whole, our Herschel flux measurements agree well with archival values. We find that the exponential horizontal dust distribution model often used in the literature generally provides a good description of the observed horizontal profiles. Three out of the seven galaxies show signatures of extended vertical emission at 100 and 160 μm at the 5σ level, but in two of these it is probably due to deviations from an exactly edge-on orientation. Only for NGC 4013, a galaxy in which vertically extended dust has already been detected in optical images, we can detect vertically extended dust, and the derived scaleheight agrees with the value estimated through radiative transfer modelling. Our analysis hints at a correlation between the dust scaleheight and its degree of clumpiness, which we infer from the difference between the dust masses as calculated from modelling of optical data and from fitting the spectral energy distribution of Herschel datapoints.

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“…We use the sample of Bureau & Freeman (1999; see also Bureau 1998), consisting of 30 edge-on spiral galaxies selected from the catalogs of Jarvis (1986), Shaw (1987), and de Souza & dos Anjos (1987; disk galaxies with a B/ PS bulge), and from that of Karachentsev, Karachentseva, & Parnovsky (1993; galaxies with extreme axial ratios). All objects are visible from the south ( P15 ) and have bulges larger than 0A6 in diameter, to have enough spatial resolution to resolve the expected bar signatures with moderate seeing.…”

Section: Samplementioning

confidence: 99%

“…However, on the whole, the sample is not biased either against or for galaxies in a dense environment. Of the 30 galaxies, 24 were identified to have a B/ PS bulge by Jarvis (1986), Shaw (1987), and de Souza & dos Anjos (1987). The other six galaxies were also selected from those catalogs but show more varied morphologies, mostly spheroidal.…”

Section: Samplementioning

confidence: 99%

Stellar Kinematics of Boxy Bulges: Large-Scale Bars and Inner Disks

2004

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Long-slit stellar kinematic observations were obtained along the major axis of 30 edge-on spiral galaxies, 24 with a boxy or peanut-shaped (B/PS) bulge and six with other bulge types for comparison. Such B/ PS bulges are identified in at least 45% of highly inclined systems, and a growing body of theoretical and observational work suggests that they are the edge-on projection of thickened bars. Profiles of the mean stellar velocity V, the velocity dispersion , as well as the asymmetric (h 3 ) and symmetric (h 4 ) deviations from a pure Gaussian are presented for all objects. Comparing these profiles with stellar kinematic bar diagnostics developed from N-body simulations, we find bar signatures in 24 of our sample galaxies (80%). Galaxies with a B/ PS bulge typically show a double-humped rotation curve with an intermediate dip or plateau. They also frequently show a rather flat central velocity dispersion profile accompanied by a secondary peak or plateau, and numerous galaxies have a local central minimum (k40%). The h 3 profiles display up to three slope reversals. Most importantly, h 3 is normally correlated with V over the presumed bar length, contrary to expectations from axisymmetric disks. These characteristic bar signatures strengthen the case for a close relationship between B/ PS bulges and bars and leave little room for other explanations of the bulges' shape. We also find that h 3 is anticorrelated with V in the very center of most galaxies (k60%), indicating that these objects additionally harbor cold and dense decoupled (quasi-) axisymmetric central stellar disks, which may be related to the central light peaks. These central disks coincide with previously identified star-forming ionized-gas disks (nuclear spirals) in gas-rich systems, and we argue that they formed out of gas accumulated by the bar at its center through inflow. As suggested by N-body models, the asymmetry of the velocity profile (h 3 ) appears to be a reliable tracer of asymmetries in disks, allowing us to discriminate between axisymmetric and barred disks seen in projection. B/ PS bulges (and thus a large fraction of all bulges) appear to be made up mostly of disk material, which has acquired a large vertical extent through bar-driven vertical instabilities. Their formation is thus probably dominated by secular evolution processes rather than merging.

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A search for box- or peanut-shaped bulges

Cited by 69 publications

References 0 publications

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

FitSKIRT: genetic algorithms to automatically fit dusty galaxies with a Monte Carlo radiative transfer code

HERschelObservations of Edge-on Spirals (HEROES)

Stellar Kinematics of Boxy Bulges: Large-Scale Bars and Inner Disks

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