J/A+A/658/A148 K corrections as a function of stellar param. (Anderson, 2022)
Relativistic corrections for measuring Hubble's constant to 1% using stellar
standard candles.
Anderson R.I.
<Astron. Astrophys. 658, A148 (2022)>
=2022A&A...658A.148A 2022A&A...658A.148A (SIMBAD/NED BibCode)
ADC_Keywords: Models ; Photometry
Keywords: distance scale - stars: variables: Cepheids - stars: distances -
relativistic processes - methods: observational - dust, extinction
Abstract:
Relativistic corrections are estimated for classical Cepheids and the
Tip of the Red Giant Branch (TRGB stars), to enable future unbiased 1%
measurements of Hubble's constant, H0. We considered four effects: K
corrections, time-dilation, the apparent change of host dust
extinction due to non-comoving reference frames, and the change of
observed color due to redshift. Extinction-dependent K corrections
were computed using stellar atmosphere models applicable to giant
stars for 0.005<z<0.030 in HST, JWST, and 2MASS filters. The
optical-NIR Wesenheit function advantageously combines filters with
oppositely signed K-corrections and avoids complications due to host
extinction. For TRGB stars, the JWST/NIRCAM F277W filter combines
insensitivity to reddening with K corrections <1% at Coma cluster
distances. Missing corrections for host extinction due to
circumgalactic or circumstellar material are discussed as potential
systematics for TRGB distances although their impacts are insufficient
to explain differences between H0 based on Cepheid or TRGB supernova
calibrations. All stellar standard candles require relativistic
corrections to achieve an unbiased 1% H0 measurement in the future.
The combined relativistic correction involving K, redshift-Leavitt
bias, and the redshift-dependence of the Wesenheit function yield an
increase of the Cepheid-based H0 by 0.45±0.05km/s/Mpc to
73.65±1.30km/s/Mpc and raises the tension with the Planck value from
4.2 to 4.4 sigma. For TRGB stars, we estimate a ∼0.5% increase of H0
reported by Freedman et al. (to 70.2±1.7km/s/Mpc) and a small
decrease by -0.15% for H0 reported by Anand et al. (to
71.4±1.8km/s/Mpc). The opposite sign of these corrections is due to
different reddening systematics and reduces the difference between the
studies by ∼0.46km/s/Mpc.
The optical-NIR Wesenheit function is particularly attractive for
accurate distance measurements because it advantageously combines
measurements in filters where K-corrections have opposite signs.
The JWST/NIRCAM F277W filter is of particular interest for TRGB stars
thanks to its insensitivity to (weak) host reddening and
K-corrections below the level of 1% at Coma cluster distances.
Description:
The tables provided here are the full versions of the tables shown as
excerpts in the Appendix as Tables A.1, A.2, and A.3.
tablea1.dat : the full grid of K corrections and apparent extinction
corrections computed using pysynphot. Foreground and calibration color
excesses are assumed to be corrected, i.e., E(B-V)fg=E(B-V)cal=0.
tablea2.dat : Three relativistic corrections applicable to a fiducial
10d Cepheid observed in the NIR Wesenheit formalism using HST/WFC3
F160W (H), F555W (V), and F814W (I). This assumes E(B-V)fg=0.023mag
and E(B-V)cal=0.4mag.
tablea3.dat : K corrections for stars near the TRGB in low-metallicity
environments for a range of host extinction values, assuming that
foreground and calibration reddening is perfectly corrected, i.e.,
E(B-V)fg=E(B-V)cal=0mag.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 150 77220 *K-corrections as a function of stellar
parameters, redshift, and reddening
tablea2.dat 31 54 *Relativistic corrections for fiducial 10d
Cepheids observed using Wesenheit magnitudes
tablea3.dat 73 3456 *K-corrections for TRGB stars
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Note on tablea1.dat: full grid of K corrections and apparent extinction
corrections computed using pysynphot. Foreground and calibration color
excesses are assumed to be corrected, i.e., E(B-V)fg=E(B-V)cal=0.
Note on tablea2.dat: Three relativistic corrections applicable to a fiducial
10d Cepheid observed in the NIR Wesenheit formalism using HST/WFC3
F160W (H), F555W (V), and F814W (I). This assumes E(B-V)fg=0.023mag
and E(B-V)cal=0.4mag.
Note on tablea3.dat: K corrections for stars near the TRGB in low-metallicity
environments for a range of host extinction values, assuming that
foreground and calibration reddening is perfectly corrected, i.e.,
E(B-V)fg=E(B-V)cal=0mag.
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 K Teff [3500/6000] effective temperature Teff
6- 8 F3.1 [cm/s2] logg [0.0/2.0] surface gravity log(g)
10- 14 F5.2 [Sun] [Fe/H] [-2.0/0.5] Iron abundance [Fe/H]
relative to Solar
16- 20 F5.3 --- z [0.0/0.03] Redshift z
22- 25 F4.2 mag E(B-V) [0.0/0.5] Host color excess E(B-V)
27- 32 F6.3 mag F555WK [-0.21/1.61] Extinction-dependent K-correction
in HST WFC3/F555W
34- 39 F6.3 mag F555WA [0.0/1.61] Extinction correction based on
apparent color excess in HST WFC3/F555W
41- 46 F6.3 mag F814WK [-0.16/0.92] Extinction-dependent K-correction
in HST WFC3/F814W
48- 53 F6.3 mag F814WA [0.0/0.911] Extinction correction based on
apparent color excess in HST WFC3/F814W
55- 60 F6.3 mag F160WK [-0.11/0.32] Extinction-dependent K-correction
in HST WFC3/F160W
62- 67 F6.3 mag F160WA [0.0/0.312] Extinction correction based on
apparent color excess in HST WFC3/F160W
69- 74 F6.3 mag JmagK [-0.07/0.45] Extinction-dependent K-correction
in 2MASS J-band
76- 81 F6.3 mag JmagA [0.0/0.436] Extinction correction based on
apparent color excess in 2MASS J-band
83- 88 F6.3 mag KsmagK [-0.05/0.22] Extinction-dependent K-correction
in 2MASS Ks-band
90- 95 F6.3 mag KsmagA [0.0/0.179] Extinction correction based on
apparent color excess in 2MASS Ks-band
97-102 F6.3 mag F115WK [-0.07/0.51] Extinction-dependent K-correction
in JWST NIRCAM/F115W
104-109 F6.3 mag F115WA [0.0/0.497] Extinction correction based on
apparent color excess in JWST NIRCAM/F115W
111-116 F6.3 mag F150WK [-0.09/0.34] Extinction-dependent K-correction
in JWST NIRCAM/F150W
118-123 F6.3 mag F150WA [0.0/0.329] Extinction correction based on
apparent color excess in JWST NIRCAM/F150W
125-129 F5.3 mag F200WK [0.0/0.240] Extinction-dependent K-correction
in JWST NIRCAM/F200W
131-136 F6.3 mag F200WA [0.0/0.214] Extinction correction based on
apparent color excess in JWST NIRCAM/F200W
138-143 F6.3 mag F277WK [-0.01/0.26] Extinction-dependent K-correction
in JWST NIRCAM/F277W
145-150 F6.3 mag F277WA [0.0/0.180] Extinction correction based on
apparent color excess in JWST NIRCAM/F277W
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 K Teff [5400] Effective Temperature
6- 8 F3.1 [cm/s2] logg [1.5] surface gravity
10- 12 F3.1 [Sun] [Fe/H] Iron abundance relative to Solar
14- 18 F5.3 --- z [0.0/0.03] Redshift
20- 23 F4.2 mag E(B-V) Host color excess
25- 26 I2 mmag W(HVI)K [2/10] NIR Wesenheit (WH,VI) K-correction
28- 29 I2 mmag DmuRLB [7/42] Redshift-Leavitt bias due to
time dilation
31 I1 mmag DmuRW [1/4] Reddening slope-Wesenheit bias
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 K Teff [3800/4500] Effective temperature
6- 8 F3.1 [cm/s2] logg Surface gravity
10- 14 F5.2 [-] [Fe/H] [-2.0/-1.5] Iron abundance relative to Solar
16- 20 F5.3 --- z [0.0/0.03] Redshift
22- 26 F5.3 mag E(B-V) Host color excess
28- 30 I3 mmag W(HVI)K [-33/4] NIR Wesenheit (WH,VI) K-correction
32- 35 I4 mmag F555WK [-173/140] Extinction-dependent K-correction
in HST WFC3/F555W
37- 39 I3 mmag F814WK [-65/86] Extinction-dependent K-correction
in HST WFC3/F814W
41- 43 I3 mmag F160WK [-76/26] Extinction-dependent K-correction
in HST WFC3/F160W
45- 48 I4 mmag F606WK [-138/126] Extinction-dependent K-correction
in HST ACS/F606W
50- 52 I3 mmag F814W2K [-65/86] Extinction-dependent K-correction
in HST ACS/F814W
54- 56 I3 mmag JmagK [-55/39] Extinction-dependent K-correction
in 2MASS J-band
58- 59 I2 mmag KsmagK [5/49] Extinction-dependent K-correction
in 2MASS Ks-band
61- 63 I3 mmag F115WK [-53/45] Extinction-dependent K-correction
in JWST NIRCAM/F115W
65- 67 I3 mmag F150WK [-74/28] Extinction-dependent K-correction
in JWST NIRCAM/F150W
69- 70 I2 mmag F200WK [4/47] Extinction-dependent K-correction
in JWST NIRCAM/F200W
72- 73 I2 mmag F277WK [2/43] Extinction-dependent K-correction
in JWST NIRCAM/F277W
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Acknowledgements:
Richard I. Anderson, richard.anderson(at)epfl.ch
(End) Patricia Vannier [CDS] 29-Jan-2022