J/ApJS/247/11 RV photon limits of well-characterized F-M stars (Reiners+, 2020)
Radial velocity photon limits for the dwarf stars of spectral classes F-M.
Reiners A., Zechmeister M.
<Astrophys. J. Suppl. Ser., 247, 11 (2020)>
=2020ApJS..247...11R 2020ApJS..247...11R
ADC_Keywords: Stars, dwarfs; Spectroscopy; Stars, distances; Stars, masses;
Effective temperatures; Magnitudes; Optical; Infrared sources
Keywords: Radial velocity; High resolution spectroscopy; G dwarf stars;
K dwarf stars; M dwarf stars; Exoplanets; Catalogs
Abstract:
The determination of extrasolar planet masses with the radial velocity
(RV) technique requires spectroscopic Doppler information from the
planet's host star, which varies with stellar brightness and
temperature. We analyze the Doppler information in spectra from dwarfs
of spectral types F-M utilizing empirical information from HARPS and
CARMENES data and model spectra. We revisit the question of whether
optical or near-infrared instruments are more efficient for RV
observations in low-mass stars, and we come to the conclusion that an
optical setup (BVR bands) is more efficient than a near-infrared one
(YJHK) in dwarf stars hotter than 3200K. We publish a catalog of 46480
well-studied F-M dwarfs in the solar neighborhood, and we compare its
distribution to more than 1 million stars from Gaia DR2. For all
stars, we estimate the RV photon noise achievable in typical
observations under the assumption of no activity jitter and slow
rotation. We find that with an ESPRESSO-like instrument at an 8m
telescope, a photon noise limit of 10cm/s or lower can be reached in
more than 280 stars in a 5 minute observation. At 4m telescopes, a
photon noise limit of 1m/s can be reached in a 10 minute exposure in
approximately 10000 predominantly Sun-like stars with a HARPS-like
(optical) instrument. The same applies to ∼3000 stars for a red
optical setup that covers the R and I bands and ∼700 stars for a
near-infrared instrument. For the latter two, many of the targets are
nearby M dwarfs. Finally, we identify targets in which Earth-mass
planets within the liquid water habitable zone can cause RV amplitudes
comparable to the RV photon noise. Assuming the same exposure times as
above, we find that an ESPRESSO-like instrument can reach this limit
for 1M⊕ planets in more than 1000 stars. The optical, red
optical, and near-infrared configurations reach the limit for
2M⊕ planets in approximately 500, 700, and 200 stars,
respectively. An online tool is provided to estimate the RV photon
noise as a function of stellar temperature and brightness and
wavelength coverage.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 135 46482 Catalog of F-M stars
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See also:
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
V/117 : Geneva-Copenhagen Survey of Solar neighbourhood (Holmberg+, 2007)
J/ApJS/101/117 : UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995)
J/A+A/337/403 : Low-mass stars evolutionary models (Baraffe+ 1998)
J/A+A/507/487 : GJ 581 radial velocity curve (Mayor+, 2009)
J/ApJ/705/1416 : Volume-limited sample of M7-M9.5 dwarfs <20pc (Reiners+, 2009)
J/AJ/143/93 : Rotational velocities in early-M stars (Reiners+, 2012)
J/A+A/556/A126 : GJ667C Doppler & activity measurements (Anglada-Escude+, 2013)
J/A+A/549/A109 : HARPS XXXI. The M-dwarf sample (Bonfils+, 2013)
J/A+A/560/A4 : Rotation periods of active Kepler stars (Reinhold+, 2013)
J/MNRAS/443/L89 : Kapteyn's star spectroscopic data (Anglada-Escude+ 2014)
J/MNRAS/443/2561 : CONCH-SHELL catalog of nearby M dwarfs (Gaidos+, 2014)
J/ApJS/220/16 : SpeX NIR survey of 886 nearby M dwarfs (Terrien+, 2015)
J/ApJS/225/32 : Extended abundance analysis of cool stars (Brewer+, 2016)
J/AJ/151/59 : Cat. of Earth-Like Exoplanet Survey Targets (Chandler+, 2016)
J/A+A/600/A13 : HARPS M dwarf stars magnetic activity (Astudillo-Defru+, 2017)
J/ApJ/834/85 : Hα emission in nearby M dwarfs (Newton+, 2017)
J/AJ/156/82 : RV characterization of TESS planets (Cloutier+, 2018)
J/MNRAS/475/1960 : ESPaDOnS spectropolarimeter obs. of M dwarfs (Fouque+, 2018)
J/A+A/614/A76 : CARMENES input catalogue of M dwarfs. III. (Jeffers+, 2018)
J/A+A/615/A6 : Photospheric parameters of CARMENES stars (Passegger+, 2018)
J/A+A/612/A49 : 324 CARMENES M dwarfs velocities (Reiners+, 2018)
J/A+A/629/A80 : ESPRESSO blind RV exoplanet survey cat. (Hojjatpanah+, 2019)
Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 25 A25 --- ID Identifier (1)
27- 30 I4 K Teff [2350/7362]? Effective temperature
32- 37 F6.1 pc Dist [1.3/8251]? Distance
39- 42 F4.2 Msun Mass [0.08/6.4]? Stellar mass
44- 48 F5.2 mag Vmag [0.3/18]? Apparent V band magnitude
50- 54 F5.2 mag Jmag [3.8/13.4]? Apparent J band magnitude
56- 62 F7.3 Lsun Lum [0/240]? Stellar luminosity
64- 68 F5.2 AU HZD [0.01/14.4]? Habitable Zone radius
70- 72 A3 --- Ref Reference code (2)
74- 79 F6.2 m/s ES-RV [0.02/774]? ESPRESSO design radial velocity
limit (3)
81- 87 F7.2 m/s HA-RV [0.05/6891]? HARPS 10 min radial velocity limit (3)
89- 94 F6.2 m/s CV-RV [0.1/985]? CARMENES VIS radial velocity limit (3)
96-101 F6.2 m/s NIR-RV [0.1/803]? NIR instrument 20min radial velocity
limit (3)
103-109 F7.2 Mgeo ES-HZ [0.09/3441]? ESPRESSO design habitable zone limit
111-117 F7.2 Mgeo HA-HZ [0.2/7107]? HARPS 10 min habitable zone limit
119-126 F8.2 Mgeo CV-HZ [0.2/20715]? CARMENES VIS habitable zone limit
128-135 F8.2 Mgeo NIR-HZ [0.3/17000]? NIR instrument 20min habitable zone
limit
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Note (1): Targets are taken from the catalogues listed below, as in Table 1:
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Catalog Teff Range V range
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Chandler+ (2016, J/AJ/151/59) 3042-7199 2.4-13.7
Nordstrom+ (2004, V/117; superseded by V/130) 4613-7396 0.4-12.7
Brewer+ (2016, J/ApJS/225/32) 4702-6674 1.7-10.0
Gaidos+ (2014, J/MNRAS/443/2561) 2700-4803 6.7-17.8
Fouque+ (2018, J/MNRAS/475/1960) 2656-4718 6.9-16.6
Terrien+ (2015, J/ApJS/220/16) 3276-4523 6.8-15.9
Reiners & Basri (2009, J/ApJ/705/1416) 2350-2620
Gaia DR2 (I/345) 3344-8000 3.0-12.0
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Note (2): Reference code as follows:
Bre = Brewer et al. (2016ApJS..225...32B 2016ApJS..225...32B);
Cha = Chandler et al. (2016AJ....151...59C 2016AJ....151...59C);
Fou = Fouque et al. (2018MNRAS.475.1960F 2018MNRAS.475.1960F);
Gai = Gaidos et al. (2014MNRAS.443.2561G 2014MNRAS.443.2561G);
Nor = Nordstrom et al. (2004A&A...418..989N 2004A&A...418..989N);
R-B = Reiners & Basri (2009ApJ...705.1416R 2009ApJ...705.1416R);
Ter = Terrien et al. (2015ApJS..220...16T 2015ApJS..220...16T).
Note (3): We compute RV precision estimates for four example spectrograph
designs: (1) an ultra-high-resolution spectrograph at an 8m telescope
covering a very wide wavelength range like ESPRESSO, (2) the HARPS
design with very high resolution at visual wavelengths operating at a
4m class telescope, (3) a red optical design like CARMENES-VIS fed by
a 4m telescope, and (4) an NIR design covering wavelengths redward of
900nm like, e.g., CARMENES-NIR, SPIROU, NIRPS, and GIANO.
Spectrograph parameters as used for the RV precision estimates
(as in Table 4):
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Instrument lambda (nm) R Rel. S/N Exp. Time
---------------------------------------------------------------
ESPRESSO 380-780 140000 2 5 minutes
HARPS 380-670 110000 1 10 minutes
CARMENES-VIS 550-950 94600 1 10 minutes
NIR 980-2440 90000 1.2 10 minutes
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 21-Apr-2020