Photometric scaling relations of lenticular and spiral galaxies

By E. Laurikainen, Heikki Salo, R. Buta, Johan H. Knapen, S. Comer'on. 2010

176 citations recorded by the source corpus.

Photometric scaling relations are studied for S0 galaxies and compared with those obtained for spirals. New two-dimensional multi-component decompositions are presented for 122 early-type disc galaxies, using deep K s -band images. Combining them with our previous decompositions, the final sample consists of 175 galaxies (Near-Infrared Survey of S0s, NIRSOS: 117 SOs + 22 S0/a and 36 Sa galaxies). As a comparison sample we use the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS) of nearly 200 spirals, for which similar multi-component decompositions have previously been made by us. The improved statistics, deep images and the homogeneous decomposition method used allow us to re-evaluate the parameters of the bulges and discs. For spirals we largely confirm previous results, which are compared with those obtained for S0s. Our main results are as follows. (1) Important scaling relations are present, indicating that the formative processes of bulges and discs in S0s are coupled [e.g. M 0 K (disc) = 0.63 M 0 K (bulge) -9.3], as has been found previously for spirals [for OSUBSGS spirals M 0 K (disc) = 0.38 M 0 K (bulge) -15.5; the rms deviation from these relations is 0.5 mag for S0s and spirals]. (2) We obtain median r eff /h 0 r ~ 0.20, 0.15 and 0.10 for S0, S0/a-Sa and Sab-Sc galaxies, respectively: these values are smaller than predicted by simulation models in which bulges are formed by galaxy mergers. (3) The properties of bulges of S0s are different from the elliptical galaxies, which are manifested in the M 0 K (bulge) versus r eff relation, in the photometric plane (μ 0 , n, reff ), and to some extent also in the Kormendy relation (〈μ〉 eff versus r eff ). The bulges of S0s are similar to bulges of spirals with M 0 K (bulge) < -20 mag. Some S0s have small bulges, but their properties are not compatible with the idea that they could evolve to dwarfs by galaxy harassment. (4) The relative bulge flux (B/T) for S0s covers the full range found in the Hubble sequence, even with 13 per cent having B/T < 0.15, typical for late-type spirals. (5) The values and relations of the parameters of the discs [h 0 r , M 0 K (disc), μ 0 (0)] of the S0 galaxies in NIRS0S are similar to those obtained for spirals in the OSUBSGS. Overall, our results support the view that spiral galaxies with bulges brighter than -20 mag in the K band can evolve directly into S0s, due to stripping of gas followed by truncated star formation.

Subfields: Astronomy and Astrophysics, Ecology, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/5e7c37ee63bf5962dea888251332fe0daec508a4

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Citations in the corpus

A REVISED PARALLEL-SEQUENCE MORPHOLOGICAL CLASSIFICATION OF GALAXIES: STRUCTURE AND FORMATION OF S0 AND SPHEROIDAL GALAXIES (2011, background): “Laurikainen et al. (2010) provide 85 S0 galaxies; i. e., de Vaucouleurs type T ≤ 0 and yet not elliptical and not a merger in progress (i. e., a disturbed E with shells and tidal tails).”
A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) (2015, background): “As a class of structures, barlenses were first recognized by Laurikainen et al. (2010), who used high-quality near-IR images and multi-component decompositions to establish the distinct nature of the features.”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “The fast rotators, like S0 galaxies (Laurikainen et al. 2010; Kormendy & Bender 2012), span the full range of bulge fraction as spiral galaxies (Krajnović et al. 2013a), and include some extremely flat disks.”
A CATALOG OF BULGE+DISK DECOMPOSITIONS AND UPDATED PHOTOMETRY FOR 1.12 MILLION GALAXIES IN THE SLOAN DIGITAL SKY SURVEY (2011, background): “…has long been debated in the literature (Andredakis et al. 1995; de Jong 1996; Balcells et al. 2003; Kormendy & Kennicutt 2004; Fisher & Drory 2010; Laurikainen et al. 2010), and our very large sample of free nb + disk decompositions should at first glance offer some insight on this interesting…”
THE SINFONI BLACK HOLE SURVEY: THE BLACK HOLE FUNDAMENTAL PLANE REVISITED AND THE PATHS OF (CO)EVOLUTION OF SUPERMASSIVE BLACK HOLES AND BULGES (2016, methodology): “Laurikainen et al. (2010); Vika et al. (2012); Läsker et al. (2014) did not publish their fitted b/a values, therefore we adopt the axis ratios (b/a)25 given by Hyperleda and compute Re = ae×(b/a)0.525 .”
THE MBH–LSPHEROID RELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES (2012, background): “…that of non-barred disc galaxies of similar total galaxy stellar mass (Aguerri et al. 2005; Laurikainen et al. 2007; Coelho & Gadotti 2011, but see Laurikainen et al. 2010), and that the bulge-to-total flux ratio is smaller in barred galaxies than in non-barred galaxies of the corresponding…”
The ATLAS3D project - VII. A new look at the morphology of nearby galaxies: the kinematic morphology-density relation (2011, background): “The large variation of bulge fractions of S0 and their overlap with the one of spirals was recently confirmed and accurately quantified by Laurikainen et al. (2010).”
THE HERSCHEL REFERENCE SURVEY: DUST IN EARLY-TYPE GALAXIES AND ACROSS THE HUBBLE SEQUENCE (2011, background): “In larger samples, Graham & Worley (2008) and Laurikainen et al. (2010) find values for this ratio of approximately 0.1– 0.2 for Sab-Sbc galaxies and 0.3–0.5 for S0 galaxies (their Figure 4), a somewhat larger change but still too low to explain the different dust-to-stellar-mass ratios.”
ANGULAR MOMENTUM AND GALAXY FORMATION REVISITED (2012, background): “Other studies have also found that bulges are more compact than ellipticals (Graham & Worley 2008; Gadotti 2009; Laurikainen et al. 2010; Dutton et al. 2011), but the quantitative details vary considerably, and we therefore regard our bulge scaling relations as provisional.”