The Demographics of Galactic Bulges in the SDSS Database

Kim, Keun-Ho; Oh, Sree; Jeong, Hyunjin; Aragón-Salamanca, Alfonso; Smith, Rory; Yi, Sukyoung K.

doi:10.3847/0067-0049/225/1/6

Cited by 28 publications

(43 citation statements)

References 102 publications

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“…The rms deviation in log (r e ) from the fitted relation (rms = 0.15) is larger than the one obtained by Bernardi et al (2003b) but similar to the K-band and B-band values of Falcón-Barroso et al (2002) and to the V-band value of Falcón-Barroso et al (2011), respectively. In literature there is a general agreement that the typical scatter of the FPR (rms 0.10) is independent of the photometric passband (Jorgensen et al 1996;La Barbera et al 2010;Kim et al 2016). But, it should be remarked that most works concentrate on ellipticals and lenticulars and adopt different fitting methods.…”

Section: Fundamental Planementioning

confidence: 75%

“…Moreover, we can infer that both ellipticals and bulges share the same properties when the FJR is used. The FJR down-bending highlighted in other works (Méndez-Abreu et al 2008a;Kim et al 2016) could be due to selection effects, when only high-or low-mass systems are considered. Indeed, the slope of the relation changes when galaxies with increasing values of absolute magnitudes are considered (Nigoche-Netro et al 2010).…”

Section: Faber-jackson Relationmentioning

confidence: 99%

“…3.3). Recently, Kim et al (2016) have shown that faint galaxies (−19 < M r, bulge < −17 mag) with smaller B/T have systematically lower σ than those with larger B/T . They concluded that bulges in low-B/T galaxies are rotation supported (i.e., disk-like bulges).…”

Section: Faber-jackson Relationmentioning

confidence: 99%

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No evidence for small disk-like bulges in a sample of late-type spirals

Costantin

Méndez-Abreu

Corsini

et al. 2017

A&A

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Context. About 20% of low-redshift galaxies are late-type spirals with a small or no bulge component. Although they are the simplest disk galaxies in terms of structure and dynamics, the role of the different physical processes driving their formation and evolution is not yet fully understood. Aims. We investigated whether small bulges of late-type spirals follow the same scaling relations traced by ellipticals and large bulges and if they are disk-like or classical bulges. Methods. We derived the photometric and kinematic properties of 9 nearby late-type spirals. To this aim, we analyzed the surfacebrightness distribution from the i-band images of the Sloan Digital Sky Survey and obtained the structural parameters of the galaxies from a two-dimensional photometric decomposition. We found a bulge component in 7 galaxies of the sample, while the remaining 2 resulted to be pure disk galaxies. We measured the line-of-sight stellar velocity distribution within the bulge effective radius from the long-slit spectra taken with high spectral resolution at the Telescopio Nazionale Galileo. We used the photometric and kinematic properties of the sample bulges to study their location in the Fundamental Plane, Kormendy, and Faber-Jackson relations defined for ellipticals and large bulges. Results. We found that our sample bulges satisfy some of the photometric and kinematic prescriptions for being considered disk-like bulges such as small sizes and masses with nearly exponential light profiles, small bulge-to-total luminosity ratios, low stellar velocity dispersions, and ongoing star formation. However, each of them follows the same scaling relations of ellipticals, massive bulges, and compact early-type galaxies so they cannot be classified as disk-like systems. Conclusions. We found a single population of galaxy spheroids that follow the same scaling relations, where the mass seems to lead to a smooth transition in the photometric and kinematic properties from less massive bulges to more massive bulges and ellipticals.

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Section: Fundamental Planementioning

confidence: 75%

Section: Faber-jackson Relationmentioning

confidence: 99%

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No evidence for small disk-like bulges in a sample of late-type spirals

Costantin

Méndez-Abreu

Corsini

et al. 2017

A&A

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“…For a review of the behaviour of the profile and its quantities, see Graham & Driver (2005) and references therein. As has often been the case in comprehensive structural decomposition studies of well-resolved galaxies (Anderdakis et al 1995;Baggett et al 1998;Khosroshahi et al 2000;Graham 2001;Allen et al 2006;Gadotti 2009;Simard et al 2011;Meert et al 2015;Kim et al 2016;Lange et al 2016;Fischer et al 2018), we have chosen to fit galaxies with two models: (1) a single Sérsic model with free Sérsic index n and (2) a combination of a near-exponential disc (0.5 < n < 1.5) plus a Sérsic bulge component (n free). Although the underlying radial light profile of a rotationally-supported disc is expected to follow an exponentially-declining profile (n = 1), in reality, the effects of projection, asymmetries due to interactions or the otherwise diffuse structure of outer spiral arms can cause deviations away from a true exponential profile (Pohlen et al 2002;Erwin et al 2005).…”

Section: Galaxy Light Profile Fittingmentioning

confidence: 99%

“…Their SDSS composite images confirm that these bulges are indeed blue rather than an artefact of our model fitting. The tail of bulge colours out to excessively red (g −i) colours has a less clear explanation; values as high as (g − i) 1.5 mag do not appear physically plausible (Fernández Lorenzo et al 2014;Mendel et al 2014;Kim et al 2016). These bulges are still likely to be some of the most red objects in the sample but our ability to derive a meaningful quantity is severely lessened in the regime where the bulge magnitudes in the g-band are significantly fainter than in the i-band.…”

Section: Separating Galaxy Componentsmentioning

confidence: 99%

xGASS: The impact of photometric bulges on the scatter of HI scaling relations

Cook

Cortese

Catinella

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a structural decomposition analysis of the galaxies in the extended GALEX Arecibo SDSS Survey (xGASS) using (gri ) images from the Sloan Digital Sky Survey. Utilising the 2D Bayesian light profile fitting code ProFit, we fit single-and double-component models taking advantage of a robust Markov chain Monte Carlo optimisation algorithm in which we assume a Sérsic profile for single-component models and a combination of a Sérsic bulge and near -exponential disc (0.5 n 1.5) for double-component models. We investigate the effect of bulges on the atomic hydrogen (H I) content in galaxies by revisiting the H I-to-stellar mass scaling relations with the bulge-to-total ratio measured in the ProFit decompositions. We show that, at both fixed total and disc stellar mass, more bulge-dominated galaxies have systematically lower H I masses, implying that bulge-dominated galaxies with large H I reservoirs are rare in the local Universe. We see similar trends when separating galaxies by a bulgeto-total ratio based either on luminosity or stellar mass, however, the trends are more evident with luminosity. Importantly, when controlling for both stellar mass and star formation rate, the separation of atomic gas content reduces to within 0.3 dex between galaxies of different bulge-to-total ratios. Our findings suggest that the presence of a photometric bulge has little effect on the global H I gas reservoirs of local galaxies.

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Barlenses in the CALIFA survey: Combining photometric and stellar population analyses

Laurikainen

Salo

Laine

2018

A&A

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Aims. It is theoretically predicted that the Boxy/Peanut bar components have a barlens appearance (a round central component embedded in the narrow bar) at low galaxy inclinations. Here we investigate barlenses in the Calar Alto Legacy Integral Field Area (CALIFA) survey galaxies, studying their morphologies, stellar populations and metallicities. We show that, when present, barlenses account for a significant portion of light of photometric bulges (i.e. the excess light on top of the disks), which highlights the importance of bars in accumulating the central galaxy mass concentrations in the cosmic timescale. Methods. We make multi-component decompositions for a sample of 46 barlens galaxies drawn from the CALIFA survey (Sánchez, García-Benito & Zibetti 2016), with M /M = 10 9.7 -10 11.4 and z = 0.005-0.03. Unsharp masks of the Sloan Digital Sky Survey (SDSS) r'-band mosaics are used to identify the Boxy/Peanut/X features. Barlenses are identified in the images using the simulation snapshots by Salo & Laurikainen (2017) as an additional guide. Our decompositions with GALFIT include in addition to bulges, disks and bars, also barlenses as a separate component. For 26 of the decomposed galaxies the CALIFA DR2 V500 grating data-cubes are used to explore the stellar ages and metallicities, at the regions of various structure components. Results. We find that 25 ± 2% of the 1064 galaxies in the whole CALIFA sample show either X-shape or barlens feature. In the decomposed galaxies with barlenses, on average 13%±2% of the total galaxy light belongs to this component, leaving less than 10% for possible separate bulge components. Most importantly, bars and barlenses are found to have similar cumulative stellar age and metallicity distributions. The metallicities in barlenses are on average near solar, but exhibit a large range. In some of the galaxies barlenses and X-shape features appear simultaneously, in which case the bar-origin of the barlens is unambiguous. Conclusions. This is the first time that a combined morphological and stellar population analysis is used to study barlenses. We show that their stars are accumulated in a prolonged time period, concurrently with the evolution of the narrow bar.

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The Demographics of Galactic Bulges in the SDSS Database

Cited by 28 publications

References 102 publications

No evidence for small disk-like bulges in a sample of late-type spirals

No evidence for small disk-like bulges in a sample of late-type spirals

xGASS: The impact of photometric bulges on the scatter of HI scaling relations

Barlenses in the CALIFA survey: Combining photometric and stellar population analyses

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