J/ApJS/266/6 In the Trenches of the solar-stellar connection. VII. (Ayres, 2023)
In the Trenches of the Solar-Stellar Connection.
VII. Wilson-Bappu 2022.
Ayres T.
<Astrophys. J. Suppl. Ser., 266, 6 (2023)>
=2023ApJS..266....6A 2023ApJS..266....6A
ADC_Keywords: Sun; Spectra, ultraviolet; Abundances, [Fe/H]; Photometry;
Optical; Spectral types; Stars, masses; Stars, diameters;
Radial velocities; Effective temperatures
Keywords: Stellar spectral lines ; Stellar radii ; Stellar masses ;
Stellar luminosities ; Stellar effective temperatures ;
Stellar activity ; Solar activity ; Stellar chromospheres
Abstract:
The Wilson-Bappu effect (WBE) is a remarkable correlation between the
width of the chromospheric emission core of the CaII 3934Å K line
and stellar absolute visual magnitude over an astonishing range, from
diminutive red dwarfs to bloated yellow supergiants. The WBE signifies
a deep connection between the nonclassical, mechanically heated
chromosphere and fundamental stellar properties. The present study
considers the parallel WBE in the analogous MgII k line at 2796Å,
utilizing near-ultraviolet spectra from Hubble Space Telescope (HST),
and stellar parameters mainly derived from Gaia. The final sample is
300 stars (301 including the Sun). The high cosmic abundance of
magnesium allowed MgII k emissions to be recovered in the warmer
F-types, at the edge of convection and chromospheric activity, and in
low-activity Sunlike dwarfs-situations in which CaII K might be too
weak to measure. Nevertheless, the derived slope of the MgII WBE was
similar to previous reports based on the K line; as well as other MgII
efforts with smaller samples of pre-HST spectra. Further, a
decomposition of the MgII WBE in temperature, gravity, activity, and
metallicity yielded similar results to previous CaII work, but with
the greater clarity afforded by the large, diverse HST sample.
Parametric dependences of the k-line WBE match, tolerably well,
predictions based on the "ionization-valve" theory of chromospheric
structure. In the end, the WBE is not merely an astrophysical
curiosity, but rather informs the question of how chromospheres-arguably
the central bastion of nonclassical heating-have come to be.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table3.dat 111 301 Stellar parameters
table4.dat 130 307 Mg II profile measurements
tablea1.dat 185 855 HST NUV exposure log
tableb1.dat 98 300 Consolidated stellar parameters
--------------------------------------------------------------------------------
See also:
B/pastel : The PASTEL catalogue (Soubiran+, 2016-)
B/hst : HST Archived Exposures Catalog (STScI, 2007)
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
J/PASP/111/335 : CaII-Mv Wilson-Bappu Effect (Wallerstein+ 1999)
J/A+A/374/1085 : Mg II K line Wilson-Bappu relationship (Cassatella+, 2001)
J/A+A/401/997 : Wilson-Bappu relation in late-type stars (Pace+, 2003)
J/A+A/398/647 : Rotational velocities of F and G stars (Reiners+, 2003)
J/A+A/430/303 : MgII-K line fluxes in active & quiet stars (Cardini+, 2005)
J/ApJ/663/320 : IR-through-UV extinction curve (Fitzpatrick+, 2007)
J/MNRAS/414/418 : Chromospheric Mg II h+k flux of evolved stars (Perez+, 2011)
J/ApJ/786/97 : Photospheric properties of T Tauri stars (Herczeg+, 2014)
J/AJ/153/212 : Obs. of binary stars at the WIYN telescope (Horch+, 2017)
J/ApJS/255/16 : Quiet-Sun MgII h & k line profiles from IRIS (Gunar+, 2021)
J/A+A/649/A3 : Gaia EDR3 photometric passbands (Riello+, 2021)
J/A+A/663/A4 : Mean PASTEL atmospheric parameters (Soubiran+, 2022)
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- f_ID [T] T = Representative T-Tauri star
3- 14 A12 --- ID Object identifier
16- 21 A6 --- SpT Spectral type / luminosity class
23- 30 F8.3 pc Dist [1.3/1000] Distance
32- 37 F6.3 mag Gmag [-0.64/14.43] Gaia DR3 G band magnitude
39- 43 F5.3 mag BP-RP [0.27/4.2] Gaia DR3 (Blue-Red) passband color
45- 49 F5.3 mag E(BP-RP) [0/0.31] Color excess, E(BP-RP)
51- 54 I4 K Teff [2888/7434]? Effective temperature (1)
56- 58 I3 K e_Teff [0/526]? Uncertainty in Teff
60 I1 --- o_Teff [1/3]? Number of values used to derive Teff
62- 66 F5.2 [Sun] [Fe/H] [-2.85/0.55]? Mean metallicity
68- 69 I2 --- o_[Fe/H] [1/32]? Number of values used to derive [Fe/H]
71- 76 F6.3 mag BC [-2.1/0.15] Bolometric correction
78- 85 E8.2 mW/m2 Fbol [9.5e-11/0.0004] Stellar bolometric flux;
erg/s/cm2 (2)
87- 92 F6.3 [Lsun] logL [-3.15/5.54] Log stellar luminosity
94- 99 F6.3 [Rsun] logR [-0.98/3.28] Log stellar radius
101- 105 F5.2 Msun Mass [0.16/24] Stellar mass
107- 111 F5.2 [cm/s2] logg [-0.73/5.6] Log surface gravity from HRD
fitting (3)
--------------------------------------------------------------------------------
Note (1): Average of up to three temperatures, TCAT, TTIC, and TCAL,
taken from Table B1.
Note (2): As calculated using a formula given in Paper VI.
Note (3): From Table B1, which was preferred over the catalog average
listed in that table.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- f_ID [T] T = Representative T-Tauri star
3- 14 A12 --- ID Object identifier
16 I1 --- Ns [1/6] Smoothing FWHM (1)
18- 23 F6.1 km/s RVCat [-317.9/252.1]? Catalog radial velocity
25 A1 --- f_RVCat [G] G: RVCat is from Gaia
27- 32 F6.1 km/s RVCal [-315/250.5] Inferred velocity shift (2)
34- 52 A19 0.1nm Min-Win Wavelength search limits for k_1 and h_1 (3)
54- 64 A11 0.1nm FIT-Win Wavelength limits used in h-line stretching (3)
66 A1 --- f_FIT-Win [rl] Flag on FIT-Win (4)
68- 71 F4.2 --- dellam [0.88/1.6] H-line δλ stretching
parameter
73- 76 F4.2 --- delf [0.94/2.2] H-line δf stretching
parameter
78- 81 F4.2 0.1nm W05 [0.27/6.43] Base profile width; Angstroms
83- 86 F4.2 0.1nm W50 [0.16/3.5] Middle profile width (FWHM);
Angstroms
88- 91 F4.2 0.1nm W95 [0/2.4] Top profile width; Angstroms
93- 100 E8.2 mW/m2 fLo [4.3e-16/0.00013] Uncorrected profile flux
measurement (5)
102- 109 E8.2 mW/m2 fUp [5e-16/0.00013] Reflected profile flux
measurement (5)
111- 118 E8.2 mW/m2 f1 [0/1.1e-05] Flux under profile base (5)
120 A1 --- Q Grade assigned (A=best) (6)
122- 130 A9 --- Sun Sun remarks (7)
--------------------------------------------------------------------------------
Note (1): In units of resels where 1 resel=2 pixels.
Note (2): Derived from the profile reflection strategy.
Note (3): Leading pair is for the k line, second is for h. The limits are with
respect to the RV-corrected laboratory wavelength: negative values
indicate the short-wavelength ("left" or "blue") side of the profile;
positive values indicate the long-wavelength ("right" or "red") side.
If the h-line values are missing, the fit was applied solely to the k
line.
Note (4):
l|r = left|right profile peak was specifically designated for the profile
reflection procedure, to override the default choice (brighter
of the two peaks).
Note (5): In units of erg/s/cm2. The reported fluxes have been corrected
for the NUV reddening.
Note (6): Assigned by visual assessment of the numerical fit; "A" is best and
"D" is worst.
Note (7): Spatially resolved IRIS intensity spectra, from the quiet Sun ("QS")
or active regions ("AR"); or based on a disk-average flux spectrum from
Gunar+ (2021ApJ...255...16G 2021ApJ...255...16G ; "FLXG"). The solar fluxes (Columns fLo,
fUp and f1) are quoted in f/fBOL units.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- ID Adopted target identifier
14 A1 --- f_ID [R] Target retained in final survey
16- 38 A23 --- SName SIMBAD name
40- 47 A8 --- Stype SIMBAD object type
49- 57 F9.5 deg RAdeg Right Ascension in decimal degrees (J2000) (1)
59- 67 F9.5 deg DEdeg [-80/86.5] Declination (J2000) (1)
69- 74 F6.2 mas Plx [1/768.1] Gaia DR3 (or Hipparcos) parallax
76- 81 F6.3 mag Gmag [1.94/16.2]? Gaia DR3 G band magnitude
83- 98 A16 --- SpT SIMBAD spectral type / luminosity class
100-120 A21 --- Note Additional note (s) (2)
122-130 A9 --- HST HST observation identifier
132-133 A2 --- f_HST Flag on HST observation (3)
135-142 F8.3 yr Tstart [1991.29/2022.64] Universal Time start date in
decimal years
144-149 A6 --- Mode Observing mode abbreviation (see text)
151-156 A6 --- Aper Spectrograph aperture abbreviation (see text)
158-162 I5 s Texp [0/11908] Exposure time
164-166 I3 --- S/NTot [0/223] Average S/N per resel outside h+k (4)
168-171 I4 --- S/Nhk [0/3803] Combined S/N of h+k lines (5)
173-179 F7.3 10-12 Fmax [0/500] Maximum flux density in h+k core region
(6)
181-185 I5 --- Nexp [1/2396] Number of sub-exposures
--------------------------------------------------------------------------------
Note (1): Epoch 2000.
Note (2): Non-flagged objects (blank in Column 2) were eliminated for reasons
summarized in the Column 10 Note:
low-S/N = Noisy hk profile;
weak = Target with adequate S/N in the hk region, but low-contrast
emission cores unsuitable for measurement;
complex = Serious inconsistency between the h and k profiles, most
common among the Mira variables;
double = Spectrally resolved binary components;
CE lim = Exceeded reddening limit.
Note (3): Flag as follows:
C = "Consensus" exposure that was retained for further consideration,
including co-addition if warranted;
a = Listed as HD 131156B in the HST catalog, but the spectrum
is of HD 131156A.
Note (4): Of the total echellegram. This value indicates the quality of the
broad NUV spectrum, excluding the Mg II core region. Specifically
for STIS, it was used as a switch to control one step of the
post-processing sequence (an iterative blaze correction).
Note (5): Based on the total net counts of h+k, taken ±2Å around
each line center, ignoring the noise contribution of the background
(normally small, but was enhanced for the STIS NUV during 2009-2015).
This metric was helpful to identify exposures that might
be weak in a global sense, but still had useable hk profiles.
Note (6): In a slightly smoothed version of the spectrum. This metric tracks
variability within a set of similar exposures, due to intrinsic
stellar chromospheric changes (or transient flares); transmission
fluctuations in a narrow slit owing to OTA "breathing;" or an
observation affected by acquisition problems.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tableb1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 A12 --- ID Adopted target identifier
14- 29 A16 --- SName SIMBAD name
31- 36 A6 --- SpT Spectral type / luminosity class
38 A1 --- f_SpT [r] Flag on SpLum (1)
40- 44 F5.2 [Sun] [Fe/H] [-2.85/0.55]? Average catalog metallicity
46- 49 F4.2 [Sun] e_[Fe/H] [0/0.4]? Uncertainty in [Fe/H]
51- 52 I2 --- o_[Fe/H] [1/32]? Number of values used to derive [Fe/H]
54- 57 I4 K TCat [2777/7447]? Average catalog effective
temperature
59- 61 I3 K e_TCat [0/204]? Uncertainty in TCat
63- 64 I2 --- o_TCat [1/38]? Number of values used to derive TCat
66- 69 I4 K TTIC [2860/7557]? TIC effective temperature
71- 73 I3 K e_TTIC [0/310]? Uncertainty in TTIC
75- 78 I4 K TCal [3000/7300] Effective temperature from
reddening-corrected Gaia color
80- 84 F5.2 [cm/s2] loggCat [0/5.25]? Average catalog log surface gravity
86- 89 F4.2 [cm/s2] e_loggCat [0/0.8]? Uncertainty in loggCat
91- 92 I2 --- o_loggCat [1/32]? Number of values used to derive
loggCat
94- 98 F5.2 [cm/s2] loggCal [-0.73/5.6] Log surface gravity from HRD
fitting
--------------------------------------------------------------------------------
Note (1): Flag as follows:
r = revised spectral type / luminosity class estimated from the effective
temperature and surface gravity if the SIMBAD classification was
discrepant (if no flag, the SIMBAD classification is listed).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Ayres T.R. Paper I. 2020ApJS..250...16A 2020ApJS..250...16A
Ayres T.R. Paper II. 2021ApJ...908..205A 2021ApJ...908..205A
Ayres T.R. Paper III. 2021ApJ...910...71A 2021ApJ...910...71A
Ayres et al. Paper IV. 2021ApJ...916...36A 2021ApJ...916...36A
Ayres T.R. Paper V. 2021ApJ...923..192A 2021ApJ...923..192A
Ayres et al. Paper VI. 2022ApJS..263...41A 2022ApJS..263...41A
Ayres T. Paper VII. 2023ApJS..266....6A 2023ApJS..266....6A This catalog
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 24-Jul-2023