J/A+A/632/A59   CALIFA galaxies stellar angular momentum (Falcon-Barroso+, 2019)

The CALIFA view on stellar angular momentum across the Hubble sequence. Falcon-Barroso J., Van De Ven G., Lyubenova M., Mendez-Abreu J., Aguerri J.A.L., Garcia-Lorenzo B., Bekeraite S., Sanchez S.F., Husemann B., Garcia-Benito R., Gonzalez Delgado R.M., Mast D., Walcher C.J., Zibetti S., Zhu L., Barrera-Ballesteros J.K., Galbany L., Sanchez-Blazquez P., Singh R., van den Bosch R.C.E., Wild V., Bland-Hawthorn J., Cid Fernandes R., de Lorenzo-Caceres A., Gallazzi A., Marino R.A., Marquez I., Peletier R.F., Perez E., Perez I., Roth M.M., Rosales-Ortega F.F., Ruiz-Lara T., Wisotzki L., Ziegler B. <Astron. Astrophys., 632, A59 (2019)> =2019A&A...632A..59F 2019A&A...632A..59F (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Morphology Keywords: galaxies: kinematics and dynamics - galaxies: elliptical and lenticular, cD - galaxies: spiral - galaxies: structure - galaxies: evolution - galaxies: formation Abstract: We present the apparent stellar angular momentum over the optical extent of 300 galaxies across the Hubble sequence using integral-field spectroscopic (IFS) data from the CALIFA survey. Adopting the same λR parameter previously used to distinguish between slow and fast rotating early-type (elliptical and lenticular) galaxies, we show that spiral galaxies are almost all fast rotators, as expected. Given the extent of our data, we provide relations for λR measured in different apertures (e.g. fractions of the effective radius: 0.5Re, Re, 2Re), including conversions to long-slit 1D apertures. Our sample displays a wide range of λRe values, consistent with previous IFS studies. The fastest rotators are dominated by relatively massive and highly star-forming Sb galaxies, which preferentially reside in the main star-forming sequence. These galaxies reach λRe values of ∼0.85, and they are the largest galaxies at a given mass, while also displaying some of the strongest stellar population gradients. Compared to the population of S0 galaxies, our findings suggest that fading may not be the dominant mechanism transforming spirals into lenticulars. Interestingly, we find that λRe decreases for late-type Sc and Sd spiral galaxies, with values that occasionally set them in the slow-rotator regime. While for some of them this can be explained by their irregular morphologies and/or face-on configurations, others are edge-on systems with no signs of significant dust obscuration. The latter are typically at the low-mass end, but this does not explain their location in the classical (V/σ, ε) and (λRe, ε) diagrams. Our initial investigations, based on dynamical models, suggest that these are dynamically hot disks, probably influenced by the observed important fraction of dark matter within Re. Description: This paper presents the CALIFA view on the stellar angular momentum distribution for a sample of 300 galaxies across the Hubble sequence. Our dataset allows us to study the distribution of λR for different apertures (0.5Re, Re, 2Re) and provides the relationship between them, including conversions to λR computed with a long-slit along the major axis of the galaxies. Our sample also helps us to investigate the relationship between λR and different global properties of galaxies (e.g. Hubble type, absolute magnitude, u-r color, concentration index, stellar mass, and star formation rate). File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tableb1.dat 83 291 Stellar angular momentum properties of the CALIFA stellar kinematics sample -------------------------------------------------------------------------------- See also: J/A+A/597/A48 : Stellar kinematics in CALIFA survey (Falcon-Barroso+, 2017) Byte-by-byte Description of file: tableb1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 I4 --- ID CALIFA ID 6- 10 F5.3 --- eps Average ellipticity measured in the outer parts of the galaxy, using SDSS images 12- 16 F5.1 deg PA [] Average position angle measured in the outer parts of the galaxy, using SDSS images 18- 21 F4.1 deg Incl Statistical inclination (see Appendix A) 23- 24 I2 arcsec Reff Effective radius of the galaxy, measured as described in Walcher et al. (2014A&A...569A...1W 2014A&A...569A...1W) 26- 28 A3 --- Type Hubble type of the galaxy from Walcher et al. (2014A&A...569A...1W 2014A&A...569A...1W) 30- 34 F5.2 10+10Msun M* Total stellar mass of the galaxy, measured as described in Walcher et al. (2014A&A...569A...1W 2014A&A...569A...1W) 36- 41 F6.2 mag rMAG Total absolute magnitude in r-band from SDSS (Abazajian et al. 2009ApJS..182..543A 2009ApJS..182..543A) 43- 46 F4.2 --- C90/50 ? Concentration index (ratio of Petrosian radius rad90 and rad50) 48- 52 F5.2 mag u-r SDSS Petrosian u-r color index 54- 58 F5.2 Msun/yr SFR ? Star formation rate based on extinction corrected Hα measurements (Sanchez et al. 2017MNRAS.469.2121S 2017MNRAS.469.2121S) 60- 63 F4.2 --- l0.5Re Apparent stellar angular momentum, λR measured on an elliptical aperture with semi-major axis 0.5Re 65- 68 F4.2 --- lRe Apparent stellar angular momentum, λR measured on an elliptical aperture with semi-major axis Re 70- 73 F4.2 --- l2Re ? Apparent stellar angular momentum, λR measured on an elliptical aperture with semi-major axis 2Re 75- 78 F4.2 --- lRe90 Deprojected apparent stellar angular momentum, λRe,90° 80- 83 F4.2 --- (V/sig)e Ordered-over-random stellar motion (V/σ)e measured on an elliptical aperture with semi-major axis Re. We refer the reader to Falcon-Barroso et al. (2017A&A...597A..48F 2017A&A...597A..48F, Cat. J/A+A/597/A48) for further properties of the galaxies not listed here. -------------------------------------------------------------------------------- History: From electronic version of the journal
(End) Patricia Vannier [CDS] 19-Feb-2020
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