J/other/ARep/68.619 Parameters of Star Formation Regions (Gusev+, 2024)
Parameters of Star Formation Regions in galaxies NGC 3963 and NGC 7292.
Gusev A.S., Sakhibov F.Kh., Moiseev A.V., Kostiuk V.S., Oparin D.V.
<Astron. Reports, 68, 619-640 (2024)>
=2024ARep...68..619G 2024ARep...68..619G (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; H II regions ; Associations, stellar ;
Clusters, open ; Interstellar medium ; Abundances
Keywords: spiral galaxies - peculiar galaxies - star formation - HII regions -
stellar population
Abstract:
Results of a study of physical parameters of stellar population in
star formation regions in galaxies with signs of peculiarity NGC 3963
and NGC 7292 are presented. The study was carried out based on the
analysis of photometric (UBVRI bands), Hα and spectroscopic data
obtained by the authors, using evolutionary models of stellar
population. Among 157 star formation regions identified in galaxies,
the young stellar population mass estimates were obtained for 16 of
them and the age estimates were obtained for 15. The age of star
formation regions clearly correlates with the presence of emission in
the Hα line: HII regions in the galaxies are younger than
6-8Myr, and the regions without gas emission are older. The studied
objects are included in the version 3 of our catalogue of photometric,
physical and chemical parameters of star formation regions, which
includes 1667 objects in 21 galaxies. Key aspects of the technique
used to estimate the physical parameters and different relations
between observational and physical parameters of the young stellar
population in star formation regions are discussed.
Description:
We present the version 3 of our catalogue of photometric, physical
(size, mass, age) and chemical parameters of star formation regions,
which includes 1667 objects in 21 galaxies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
galaxies.dat 33 21 List of galaxies
sfr-cat3.dat 367 1667 Parameters of star formation regions
(Version 3, 10.03.2024)
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Byte-by-byte Description of file: galaxies.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Galaxy Galaxy name
11- 12 I2 h RAh Simbad right ascension (J2000)
14- 15 I2 min RAm Simbad right ascension (J2000)
17- 21 F5.2 s RAs Simbad right ascension (J2000)
23 A1 --- DE- Simbad declination sign (J2000)
24- 25 I2 deg DEd Simbad declination (J2000)
27- 28 I2 arcmin DEm Simbad declination (J2000)
30- 33 F4.1 arcsec DEs Simbad declination (J2000)
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Byte-by-byte Description of file: sfr-cat3.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Seq Serial number
6- 14 A9 --- Galaxy Galaxy name
16- 18 I3 --- No Serial number of the object within a galaxy
20- 25 F6.1 arcsec NS Apparent coordinate relative to the galaxy
centre in the plane of the sky (2)
27- 32 F6.1 arcsec EW Apparent coordinate relative to the galaxy
centre in the plane of the sky (2)
34- 38 F5.2 kpc r Deprojected galactocentric distance
40- 44 F5.3 --- r/R25 Deprojected galactocentric distance (3)
46- 50 F5.2 mag Bmag Apparent total B magnitude
52- 57 F6.2 mag BMAG Absolute magnitude in B band (4)
59- 62 F4.2 mag e_BMAG Absolute B magnitude uncertainty
64- 69 F6.2 mag U-B ?=-10 Apparent colour index U-B
71- 76 F6.2 mag e_U-B ?=-10 Uncertainty of the U-B
78- 82 F5.2 mag B-V Apparent colour index B-V
84- 87 F4.2 mag e_B-V Uncertainty of the B-V
89- 94 F6.2 mag V-R ?=-10 Apparent colour index V-R
96-101 F6.2 mag e_V-R ?=-10 Uncertainty of the V-R
103-108 F6.2 mag V-I ?=-10 Apparent colour index V-I
110-115 F6.2 mag e_V-I ?=-10 Uncertainty of the V-I
117-122 F6.2 [mW/m2] logFHa ?=100 Logarithm of spectrophotometric
flux (5)
124-129 F6.2 [mW/m2] e_logFHa ?=-10 Uncertainty of the logarithm of
spectrophotometric flux
131-136 F6.2 mag BMAG-0i Absolute magnitude, corrected for the
Galactic extinction and inclination effects
138-143 F6.2 mag U-B-0i ?=-10 Colour index U-B, corrected for the
Galactic extinction and inclination effects
145-149 F5.2 mag B-V-0i Colour index B-V, corrected for the Galactic
extinction and inclination effects
151-156 F6.2 mag V-R-0i ?=-10 Colour index V-R, corrected for the
Galactic extinction and inclination effects
158-163 F6.2 mag V-I-0i ?=-10 Colour index V-I, corrected for the
Galactic extinction and inclination effects
165-170 F6.2 [mW/m2] logFHa-0i ?=100 Logarithm of spectrophotometric flux,
corrected for the Galactic extinction and
inclination effects (5)
172-177 F6.2 --- R-Ha ?=10 R-Hα index (6)
179-180 I2 --- Ha-data [-1/2] Gas-to-stars morphology (7)
182-187 F6.2 mag A(B) ?=-10 Absorption calculated from
Balmer decrement
189-194 F6.2 mag e_A(B) ?=-10 Uncertainty of the absorption A(B)
196-201 F6.1 0.1nm EW(Ha) ?=-10 Equivalent width
203-207 F5.1 0.1nm e_EW(Ha) ?=-10 Uncertainty of the equivalent width
209-214 F6.2 [0.1nm] logEW(Ha) ?=-10 Logarithm of equivalent width
216-221 F6.2 [0.1nm] e_logEW(Ha) ?=-10 Uncertainty of the logarithm of
equivalent width
223-230 F8.4 --- Z ?=-10 Metallicity
232-239 F8.4 --- e_Z ?=-10 Uncertainty of the metallicity
241-246 F6.2 --- gas ?=-10 The relative contribution of nebular
continuum and emission lines to the total
observed flux in B band,
IB(gas)/IB(total)
248-253 F6.2 mag BMAGtr ?=100 Absolute magnitude, corrected for
extinction and nebular emission
contribution
255-260 F6.2 mag e_BMAGtr ?=-10 Uncertainty of the M_Btr
262-267 F6.2 mag U-Btr ?=-10 Colour index U-B, corrected for
extinction and nebular emission
contribution
269-274 F6.2 mag e_U-Btr ?=-10 Uncertainty of the U-Btr
276-281 F6.2 mag B-Vtr ?=-10 Colour index B-V, corrected for
extinction and nebular emission
contribution
283-288 F6.2 mag e_B-Vtr ?=-10 Uncertainty of the B-Vtr
290-295 F6.2 mag V-Rtr ?=-10 Colour index V-R, corrected for
extinction and nebular emission
contribution
297-302 F6.2 mag e_V-Rtr ?=-10 Uncertainty of the V-Rtr
304-309 F6.2 mag V-Itr ?=-10 Colour index V-I, corrected for
extinction and nebular emission
contribution
311-316 F6.2 mag e_V-Itr ?=-10 Uncertainty of the V-Itr
318-323 F6.2 [mW/m2] logIHa ?=100 Logarithm of spectrophotometric flux,
corrected for absorption A (5)
325-330 F6.2 [mW/m2] e_logIHa ?=-10 Uncertainty of the logIHα
332-337 F6.2 Myr Age ?=-10 Age
339-344 F6.2 Myr e_Age ?=-10 Uncertainty of the age
346-352 F7.2 10+4Msun Mass ?=-10 Mass
354-359 F6.2 10+4Msun e_Mass ?=-10 Uncertainty of the mass
361-364 I4 pc Diam Diameter
366-367 I2 --- str Structure (8)
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Note (2): Positive values correspond to the northern and western positions.
Note (3): Isophotal radius R_25 is corrected for the Galactic extinction and
inclination effects.
Note (4): BMAG = Bmag-5logD-25, where D is an adopted distance in units of Mpc.
Note (5): Hα+[NII] flux for all galaxies except NGC 266, 3184, 3963, and
6217, and logarithm of Hα flux for the objects in NGC 266, 3184,
3963, and 6217.
Note (6): R-Hα = R+2.5log F(Hα+[NII]) for all galaxies except NGC
266, 3184, 3963, and 6217,
R-Hα = R+2.5log F(1.35Hα) for NGC 266, 3184, and 6217,
and R-Hα = R+2.5log F(Hα+1.33[NII]6584) for NGC 3963,
where R is in magnitudes, and Hα+[NII] (Hα) are
the fluxes in units of erg/s/cm2.
Note (7): Gas-to-stars morphology as follows:
2 = Optical radiation from stars coincident with ionized gas emission
1 = Photometric (stellar) radiation centre is displaced from the gas
emission centre
0 = No gas emission within the area of optical radiation from stars
-1 = No Hα data
Note (8): Structure of star formation region as follows:
1 = Separated object with star-like profile
2 = Double object
3 = Triple object
4 = Separated object with diffuse profile
5 = Ring structure
6 = Complex structure (more than three separated objects)
10 = Separated object with star-like profile, the object is a brighter
part (core) of an more extended star forming region
20 = Double object, the object is a brighter part (core) of an more
extended star forming region
30 = Triple object, the object is a brighter part (core) of an more
extended star forming region
40 = Separated object with diffuse profile, the object is a brighter
part (core) of an more extended star forming region
50 = Ring structure, the object is a brighter part (core) of an
more extended star forming region
60 = Complex structure (more than three separated objects, the object
is a brighter part (core) of an more extended star forming region
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Acknowledgements:
Alexander Gusev, gusev(at)sai.msu.ru
References:
Gusev et al., Paper I 2016MNRAS.457.3334G 2016MNRAS.457.3334G
Gusev et al., Paper II 2023MNRAS.525..742G 2023MNRAS.525..742G
(End) Patricia Vannier [CDS] 25-Nov-2024