J/other/RAA/19.81 Blue-core galaxies properties (Chen+, 2019)
The morphology, kinematics and metallicity of blue-core galaxies.
Chen Y.-Y., Chen Y.-M., Gu Q.-S., Shi Y., Bing L.-J., Yu X.-L.
<Res. Astron. Astrophys., 19, 81 (2019)>
=2019RAA....19...81C 2019RAA....19...81C (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, optical ; Morphology
Keywords: galaxies: abundances - galaxies: formation - galaxies: structure
Abstract:
We select 107 blue-core galaxies from the MaNGA survey, studying their
morphology, kinematics as well as the gas-phase metallicity. Our
results are as follows: (i) In our sample, 26% of blue-core galaxies
have decoupled gas-star kinematics, indicating external gas accretion;
15% have bar-like structure and 8% show post-merger features, such as
tidal tails and irregular gas/star velocity field. All these
processes/features, such as accreting external misaligned gas,
interaction and bar, can trigger gas inflow. Thus the central
star-forming activities lead to bluer colors in their centers
(blue-core galaxies). (ii) By comparing with the SDSS DR7 star-forming
galaxy sample, we find that the blue-core galaxies have higher central
gas-phase metallicity than what is predicted by the local
mass-metallicity relation. We explore the origin of the higher
metallicity, finding that not only the blue-core galaxies, but also
the flat-gradient and red-core galaxies all have higher metallicity.
This can be explained by the combined effect of redshift and galaxy
color.
Description:
We select 107 blue-core galaxies from MaNGA MPL5, studying their
morphology, kinematics as well as gas phase metallicity. We summarize
the properties of blue-core galaxies in Table 1.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 76 107 The sample of blue-core galaxies
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name MaNGA ID (1-NNNNNN)
10- 21 F12.8 deg RAdeg Right ascension (J2000)
22- 34 F13.9 deg DEdeg Declination (J2000)
36- 41 F6.4 --- z Redshift
43- 47 F5.2 [Msun] logM* Stellar mass
49- 50 I2 deg i Inclination angle
52- 54 I3 deg DPA ? Difference in the kinematic PA between star
and ionized gas which is defined as
{DELTA}PA=|PAstar-PAgas| (1)
56- 58 I3 deg e_DPA ? rms uncertainty on DPA
60- 76 A17 --- Morph Morphology
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Note (1): The kinematic PA is measured based on established methods
(Krajnovic et al., 2006MNRAS.366..787K 2006MNRAS.366..787K).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 08-Aug-2019