J/ApJS/263/1 Spectrophotometry of standard stars (Rubin+, 2022)
Uniform recalibration of common spectrophotometry standard stars onto the
CALSPEC system using the SuperNova Integral Field Spectrograph.
Rubin D., Aldering G., Antilogus P., Aragon C., Bailey S., Baltay C.,
Bongard S., Boone K., Buton C., Copin Y., Dixon S., Fouchez D., Gangler E.,
Gupta R., Hayden B., Hillebrandt W., Kim A.G., Kowalski M., Kusters D.,
Leget P.-F., Mondon F., Nordin J., Pain R., Pecontal E., Pereira R.,
Perlmutter S., Ponder K.A., Rabinowitz D., Rigault M., Runge K.,
Saunders C., Smadja G., Suzuki N., Tao C., Taubenberger S., Thomas R.C.,
Vincenzi M., The Nearby Supernova Factory
<Astrophys. J. Suppl. Ser., 263, 1 (2022)>
=2022ApJS..263....1R 2022ApJS..263....1R
ADC_Keywords: Stars, standard; Spectra, optical; Spectral types; Models
Keywords: Flux calibration ; Spectrophotometry ; Spectrophotometric standards
Abstract:
We calibrate spectrophotometric optical spectra of 32 stars commonly
used as standard stars, referenced to 14 stars already on the Hubble
Space Telescope-based CALSPEC flux system. Observations of CALSPEC and
non-CALSPEC stars were obtained with the SuperNova Integral Field
Spectrograph over the wavelength range 3300-9400Å as calibration
for the Nearby Supernova Factory cosmology experiment. In total, this
analysis used 4289 standard-star spectra taken on photometric nights.
As a modern cosmology analysis, all presubmission methodological
decisions were made with the flux scale and external comparison
results blinded. The large number of spectra per star allows us to
treat the wavelength-by-wavelength calibration for all nights
simultaneously with a Bayesian hierarchical model, thereby enabling a
consistent treatment of the Type Ia supernova cosmology analysis and
the calibration on which it critically relies. We determine the
typical per-observation repeatability (median 14mmag for exposures
≥5s), the Maunakea atmospheric transmission distribution (median
dispersion of 7mmag with uncertainty 1mmag), and the scatter internal
to our CALSPEC reference stars (median of 8mmag). We also check our
standards against literature filter photometry, finding generally good
agreement over the full 12mag range. Overall, the mean of our system
is calibrated to the mean of CALSPEC at the level of ∼3mmag. With our
large number of observations, careful cross-checks, and 14 reference
stars, our results are the best calibration yet achieved with an
integral-field spectrograph, and among the best calibrated surveys.
Description:
This work presents the results from a large sample of optical
spectrophotometry of 46 stars from the SuperNova Integral-Field
Spectrograph (SNIFS) instrument on the University of Hawaii (UH) 2.2m
telescope.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 115 49 Spectrophotometric standard stars used or
considered in this analysis
table3.dat 49 2501 Atmospheric extinction in magnitudes from our
radiative-transfer model (convolved to SNIFS
resolution), evaluated at three different airmass
values
table4.dat 51 2351 Atmospheric extinction, measured vs modeled
sp/* . 46 Individual spectra in TSV format
--------------------------------------------------------------------------------
See also:
II/179 : Southern Spectrophotometric Standards. I + II (Hamuy+ 1992,94)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/A+AS/105/503 : Binary star speckle measurements (Balega+ 1994)
J/A+AS/125/497 : Theta Vir and 109 Vir uvby photometry (Adelman 1997)
J/AJ/124/1144 : Orbits of 171 single-lined sp. binaries (Latham, 2002)
J/AJ/133/768 : KPNO's UBVRI transmission characteristics (Landolt+, 2007)
J/other/AstBu/63.278 : Metal-poor stars speckle interferom. (Rastegaev+, 2008)
J/AJ/137/4186 : UBVRI standards around celestial equator (Landolt, 2009)
J/MNRAS/403/1949 : UBV(RcIc)JHK photometry of HIP nearby stars (Koen+, 2010)
J/PASP/124/140 : UBVRI Hp BT and VT photonic responses (Bessell+, 2012)
J/MNRAS/426/1767 : Gaia spectrophotometric standard stars I. (Pancino+, 2012)
J/ApJ/750/99 : The Pan-STARRS1 photometric system (Tonry+, 2012)
J/A+A/552/A124 : SNLS and SDSS SN surveys phot. calibration (Betoule+, 2013)
J/A+A/549/A8 : Atmospheric extinction above Mauna Kea (Buton+, 2013)
J/MNRAS/462/3616 : Gaia SPSS variability monitoring (Marinoni+, 2016)
J/AJ/157/229 : CALSPEC: WFC3 IR grism spectrophotometry (Bohlin+, 2019)
J/A+A/649/A3 : Gaia EDR3 photometric passbands (Riello+, 2021)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Our name
13- 15 A3 --- f_Name Flag(s) on Name (1)
17- 31 A15 --- AName Alternative name
33 A1 --- f_AName Flag on Aname (1)
35- 42 A8 --- Ref Reference (2)
44- 46 A3 --- Set Sample (3)
48- 49 I2 h RAh Hour of right ascension (J2000)
51- 52 I2 min RAm Minute of right ascension (J2000)
54- 59 F6.3 s RAs Second of right ascension (J2000)
61 A1 --- DE- Sign of declination (J2000)
62- 63 I2 deg DEd Degree of declination (J2000)
65- 66 I2 arcmin DEm Arcminute of declination (J2000)
68- 72 F5.2 arcsec DEs Arcsecond of declination (J2000)
74- 79 F6.3 mag Vmag [3.4/14.7] V magnitude
81- 92 A12 --- SpT MK spectral type
94- 96 I3 --- Nn [1/228] Number of photometric nights on which
the star was observed
98-100 I3 s Exp [1/601] Median exposure time
102-115 A14 --- File Name of the TSV file in "sp" subdirectory
--------------------------------------------------------------------------------
Note (1): Flag as follows:
c = Has companion; see Section 2.1.
d = Pancino+ (2012, J/MNRAS/426/1767) showed that Hamuy+ (1992, II/179)
misidentified this star as LTT 377.
e = Suspected variable star; see Section 2.2.
f = Variable star; see Section 2.2.
n = Excluded stars (3 occurrences)
Note (2): Source as follows:
SC = Bohlin et al. 2020AJ....160...21B 2020AJ....160...21B
SSPS = Hamuy+ 1992, 1994 (Cat. II/179)
O90 = Oke 1990AJ.....99.1621O 1990AJ.....99.1621O
Note (3): Sample as follows:
FWD = Fundamental white dwarf (3 occurrences)
P = primary CALSPEC star (11 occurrences)
S = secondary star (31 occurrences)
R = rejected (4 occurrences)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.1 0.1nm lambda [6000/11000] Wavelength, Angstroms
9- 14 F6.4 mag EXT-X1.0 [0/0.92] Median extinction for Airmass=1.0
16- 21 F6.4 mag RMS-X1.0 [0/0.13] RMS for Airmass=1.0
23- 28 F6.4 mag EXT-X1.5 [0/1.2] Median extinction for Airmass=1.5
30- 35 F6.4 mag RMS-X1.5 [0/0.17] RMS for Airmass=1.5
37- 42 F6.4 mag EXT-X2.0 [0/1.43] Median extinction for Airmass=2.0
44- 49 F6.4 mag RMS-X2.0 [0/0.2] RMS for Airmass=2.0
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 0.1nm lambda [3298.68/9701.23] Wavelength, Angstroms
9- 15 F7.4 mag EXT-MES-Med [-0.019/0.57] Median measured extinction
17- 22 F6.4 mag EXT-MES-RMS [0.005/0.041] RMS in measured extinction
24- 29 F6.4 mag EXT-MES-Unc [0.0012/0.0041] Uncertainty on mean, measured
31- 36 F6.4 mag EXT-MOD-Med [0.013/0.6] Median modeled extinction (1)
38- 43 F6.4 mag EXT-MOD-RMS [0.0038/0.024] RMS in modeled extinction (1)
45- 51 F7.4 mag EXT-MOD-Unc [-0.0009/0.0013] Uncertainty on mean,
modeled (1)
--------------------------------------------------------------------------------
Note (1): Best-fit physical model (without the constant-in-wavelength
component that appears to be linked to PSF variation and not the
atmosphere).
--------------------------------------------------------------------------------
History:
From electronic version of the journal for Tables 1, 3, 4
Spectra downloaded at: doi:10.5281/zenodo.6904580
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 22-Nov-2022