Spectral Libraries#
A number of spectral libraries have been include in speXtra.
See database-contents for a summary what is included in the database.
To list the names of the libraries included in the database
from spextra import spextra_database
spextra_database["libraries"]
/home/docs/checkouts/readthedocs.org/user_builds/spextrahb/envs/stable/lib/python3.11/site-packages/tqdm/auto.py:21: TqdmWarning: IProgress not found. Please update jupyter and ipywidgets. See https://ipywidgets.readthedocs.io/en/stable/user_install.html
from .autonotebook import tqdm as notebook_tqdm
{'ref': 'Library of reference stars',
'kc96': 'Kinney-Calzetti Atlas',
'pickles': 'Pickles Stellar Library',
'dobos': 'SDSS galaxy composite spectra',
'irtf': 'IRTF spectral library',
'agn': 'AGN templates',
'nebulae': 'Emission line nebulae',
'brown': 'Galaxy SEDs from the UV to the Mid-IR',
'kurucz': 'Subset of Kurucz 1993 Models',
'sne': 'Supernova Legacy Survey',
'moehler': 'flux/telluric standards with X-Shooter',
'madden': 'High-Resolution Spectra of Habitable Zone Planets',
'bosz/hr': 'BOSZ stellar atmosphere Grid - High Resolution',
'bosz/mr': 'BOSZ stellar atmosphere Grid - Medium Resolution',
'bosz/lr': 'BOSZ stellar atmosphere Grid - Low Resolution',
'sky': 'Paranal sky background spectra',
'shapley': 'Rest-Frame Ultraviolet Spectra of z ∼ 3 Lyman Break Galaxies',
'etc/kurucz': 'ESO ETC subset of the Kurucz 1993 models',
'etc/marcs/p': 'ESO ETC subset of the MARCS Stellar Models with Plane Parallel Geometry',
'etc/marcs/s': 'ESO ETC subset of the MARCS Stellar Models with Spherical Geometry',
'etc/misc': 'Other templates, nubulae and qso'}
To see which templates are available in each library
from spextra import SpecLibrary
lib = SpecLibrary("kc96")
list(lib)
['elliptical',
'bulge',
's0',
'sa',
'sb',
'sc',
'starb1',
'starb2',
'starb3',
'starb4',
'starb5',
'starb6']
Below you can find a detailed description of each library.
A Library of Reference Stars#
name: ref
type: stellar
title: Reference library
summary: ""
reference: ""
url: "https://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/calspec"
spectral_coverage:
- UV
- VIS
- NIR
- MIR
parameters:
resolution: 10 # [??]
wave_col: WAVELENGTH
flux_col: FLUX
file_extension: .fits
items:
vega: {waverange: [900 AA, 300 um]}
vegaLR: {waverange: [1148 AA, 2.6 um]}
sirius: {waverange: [900 AA, 300 um]}
sun: {waverange: [1195 AA, 2.7 um]}
sunHR: {waverange: [1500 AA, 300 um]}
The Kinney-Calzetti Spectral Atlas of Galaxies#
name: kc96
type: extragalactic
title: The Kinney-Calzetti Spectral Atlas of Galaxies
abstract: |
The Kinney-Calsetti Atlas consists of an homogeneous set of 12 galaxy spectral
covering the ultraviolet, optical and near-infrared wavelength range up to
about 1 micron. The spectra include various morphological types and starburst
galaxies.
This atlas contains a set of galaxy spectral covering the ultraviolet to
near-infrared spectral range (i.e. from 0.12 to 1 μm). The ultraviolet range
of the spectral templates was obtained with the large aperture (10" by 20")
and low resolution spectrographs on the IUE satellite. The optical spectra
were obtained through a long slit with a 10" width, where a window of 20" long
was extracted to match the IUE aperture.
The spectral templates cover various galaxy morphological types from
elliptical to late type spiral. Starburst spectra for low (E(B-V < 0.10) to
high (0.61 < E(B-V) < 0.70) internal extinction are also available. Several of
the starburst galaxies used are classified as irregulars. Thus, although
irregular galaxies are not explicitly covered, the starburst templates can be
used for this morphological type. Details about how the spectra have been
constructed can be found in Kinney et al. (1996) for the different
morphological types, and in Calzetti et al. (1994) for the starbursts.
The flux of the spectra has been normalized to a visual magnitude of 12.5 (STMAG).
Details about each spectrum can be found in the header of the FITS file.
reference: Kinney et al. 1996
bibcode: "1996ApJ...467...38K"
adsurl: "https://ui.adsabs.harvard.edu/abs/1996ApJ...467...38K"
doi: "10.1086/177583"
url: "http://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/the-kinney-calzetti-spetral-atlas"
spectral_coverage :
- UV
- VIS
parameters:
resolution: 10 # [??]
wave_col: WAVELENGTH
flux_col: FLUX
file_extension: .fits
items:
elliptical: []
bulge: []
s0: []
sa: []
sb: []
sc: []
starb1: [starburst, E(B-V) < 0.1]
starb2: [starburst, 0.11 < E(B-V) < 0.21]
starb3: [starburst, 0.25 < E(B-V) < 0.35]
starb4: [starburst, 0.39 < E(B-V) < 0.50]
starb5: [starburst, 0.51 < E(B-V) < 0.60]
starb6: [starburst, 0.61 < E(B-V) < 0.70]
Pickles Stellar Library#
name: pickles
type: stellar
title: Pickles Stellar Spectral Flux Library
abstract: |
This library of wide spectral coverage, consists of 131 flux calibrated
stellar spectra, encompassing all normal spectral types and luminosity classes
at solar abundance, and metal-weak and metal-rich F-K dwarf and G-K giant
components. Each spectrum in the library is a combination of several sources
overlapping in wavelength coverage. The creator of the library has followed
precise criteria in combining sources and to assembling the most reliable
spectra. As part of the selection criteria prior to combination, all input
sources were checked aginst the SIMBAD database and against the colors and
line strengths as derived by the observed spectra themselves, in order to
esure they had similar spectral types.
reference: Pickles, A. J. 1998, PASP, 110, 863
url: "https://www.eso.org/sci/facilities/paranal/decommissioned/isaac/tools/lib.html"
spectral_coverage:
- UV
- VIS
- NIR
parameters:
resolution: 5 # [AA]
wave_col: WAVELENGTH
flux_col: FLUX
file_extension: .fits
items:
o5v: ""
o8iii: ""
o9v: ""
b0i: ""
b0v: ""
b12iii: ""
b1i: ""
b1v: ""
b2ii: ""
b2iv: ""
b3i: ""
b3iii: ""
b3v: ""
b57v: ""
b5i: ""
b5ii: ""
b5iii: ""
b6iv: ""
b8i: ""
b8v: ""
b9iii: ""
b9v: ""
a0i: ""
a0iii: ""
a0iv: ""
a0v: ""
a2i: ""
a2v: ""
a3iii: ""
a3v: ""
a47iv: ""
a5iii: ""
a5v: ""
a7iii: ""
a7v: ""
f02iv: ""
f0i: ""
f0ii: ""
f0iii: ""
f0v: ""
f2ii: ""
f2iii: ""
f2v: ""
f5i: ""
f5iii: ""
f5iv: ""
f5v: ""
f6v: ""
f8i: ""
f8iv: ""
f8v: ""
rf6v: metal rich
rf8v: metal rich
wf5v: metal weak
wf8v: metal weak
g0i: ""
g0iii: ""
g0iv: ""
g0v: ""
g2i: ""
g2iv: ""
g2v: ""
g5i: ""
g5ii: ""
g5iii: ""
g5iv: ""
g5v: ""
g8i: ""
g8iii: ""
g8iv: ""
g8v: ""
rg0v: metal rich
rg5iii: metal rich
rg5v: metal rich
wg0v: metal weak
wg5iii: metal weak
wg5v: metal weak
wg8iii: metal weak
k01ii: ""
k0iii: ""
k0iv: ""
k0v: ""
k1iii: ""
k1iv: ""
k2i: ""
k2iii: ""
k2v: ""
k34ii: ""
k3i: ""
k3iii: ""
k3iv: ""
k3v: ""
k4i: ""
k4iii: ""
k4v: ""
k5iii: ""
k5v: ""
k7v: ""
rk0iii: metal rich
rk0v: metal rich
rk1iii: metal rich
rk2iii: metal rich
rk3iii: metal rich
rk4iii: metal rich
rk5iii: metal rich
wk0iii: metal weak
wk1iii: metal weak
wk2iii: metal weak
wk3iii: metal weak
wk4iii: metal weak
m0iii: ""
m0v: ""
m1iii: ""
m1v: ""
m2.5v: ""
m2i: ""
m2iii: ""
m2v: ""
m3ii: ""
m3iii: ""
m3v: ""
m4iii: ""
m4v: ""
m5iii: ""
m5v: ""
m6iii: ""
m6v: ""
m7iii: ""
m8iii: ""
m9iii: ""
m10iii: ""
SDSS galaxy composite spectra#
name: dobos
type: extragalactic
title: A High Resolution Atlas of Composite SDSS Galaxy Spectra
abstract: |
In this work we present an atlas of composite spectra of galaxies based on the
data of the Sloan Digital Sky Survey Data Release 7 (SDSS DR7). Galaxies are
classified by colour, nuclear activity and star-formation activity to
calculate average spectra of high signal-to-noise ratio and resolution
(S/N ~ 132 - 4760 at delta lambda = 1 AA), using an algorithm that is robust
against outliers. Besides composite spectra, we also compute the first five
principal components of the distributions in each galaxy class to characterize
the nature of variations of individual spectra around the averages. The
continua of the composite spectra are fitted with BC03 stellar population
synthesis models to extend the wavelength coverage beyond the coverage of the
SDSS spectrographs. Common derived parameters of the composites are also
calculated: integrated colours in the most popular filter systems, line
strength measurements, and continuum absorption indices (including Lick
indices). These derived parameters are compared with the distributions of
parameters of individual galaxies and it is shown on many examples that the
composites of the atlas cover much of the parameter space spanned by SDSS
galaxies. By co-adding thousands of spectra, a total integration time of
several months can be reached, which results in extremely low noise
composites. The variations in redshift not only allow for extending the
spectral coverage bluewards to the original wavelength limit of the SDSS
spectrographs, but also make higher spectral resolution achievable. The
composite spectrum atlas is available online at
http://www.vo.elte.hu/compositeatlas.
reference: Dobos, L.; Csabai, I; Yip, C.; Budavári, T; Wild, V; Szalay, A. 2012, MNRAS 420, 1217
bibref: ""
adsurl: ""
doi: ""
url: "http://www.vo.elte.hu/compositeatlas/v1/Default.aspx"
spectral_coverage:
- UV
- VIS
parameters:
resolution: 1 # [??]
wave_unit: Angstrom
flux_unit: FLAM
wave_col: lambda
flux_col: flux
file_extension: .dat
items:
BG: Blue
G: Green
GG: Green
h_BG: Halpha measured, Blue, Green
h_G: Halpha measured, Green
h_GG: Halpha measured, Green, Green
hh_BG: star-forming, Blue
hh_G: star-forming, Green
hh_GG: star-forming, Green
hh_RG: star-forming, Red
h_RG: Halpha measured, Red
l_BG: LINER, Blue
l_G: LINER, Green
l_GG: LINER, Green
l_RG: LINER, Red
p_BG: passive, Blue
p_G: passive, Green
p_GG: passive, Green
p_RG: passive, Red
RED0: Red 0
RED1: Red 1
RED2: Red 2
RED3: Red 3
RED4: Red 4
RG: Red
s_BG: Seyfert, Blue
SF1: Star-Forming 1
SF2: Star-Forming 2
SF3: Star-Forming 3
SF4: Star-Forming 4
s_G: Seyfert, Green
s_GG: Seyfert, Green
s_RG: Seygert, Red
t_BG: Composite, Blue Green
t_G: Composite Galaxy
t_GG: Composite, Green
t_RG: Composite, Red
IRTF spectral library#
name: irtf
type:
- stellar
- planetary
synthetic: False
title: The IRTF Spectral Library
abstract: |
The IRTF Spectral Library is a collection of 0.8-5.0 um mostly stellar spectra
observed at a resolving power of R~2000 with the medium-resolution
spectrograph, SpeX, at the NASA Infrared Telescope Facility (IRTF) on Mauna
Kea. The current release covers mainly solar-metallicity late-type stars with
spectral types between F and M and luminosity classes between I and V, but
also includes AGB stars, carbon and S stars, and L and T dwarfs. We also
include spectra of the giant planets, Jupiter, Saturn, Uranus, and Neptune.
Later updates will add Wolf-Rayet, O, B, and A stars.
reference: Rayner, Cushing, & Vacca 2009
bibcode: "2009ApJS..185..289R"
adsurl: "https://ui.adsabs.harvard.edu/abs/2009ApJS..185..289R"
doi: "10.1088/0067-0049/185/2/289"
url: "http://irtfweb.ifa.hawaii.edu/~spex/IRTF_Spectral_Library/index.html"
spectral_coverage:
- NIR
- MIR
parameters:
resolution: 0.0015 # [um]
wave_unit: um
flux_unit: W m-2 um-1
wave_col: WAVELENGTH
flux_col: FLUX
file_extension: .dat
items: # comments: star_name, spectral_type
C7: [HD31996, C7.6e(N4)]
C-J4: [HD70138, C-J4.5IIIaC26j6]
C-J5: [HD57160, C-J5-C25-j4]
C-N4.5C: [HD92055, C-N4.5C24.5]
C-N4C23: [HD44984, C-N4C23.5]
C-N5C26: [HD48664, C-N5C26-]
C-R2: [HD76846, C-R2+IIIaC22.5]
F0Ia: [HD7927_ext, F0Ia]
F0Ib: [HD135153_ext, F0Ib-II]
F0II: [HD6130_ext, F0II]
F0IIIa: [HD89025, F0IIIa]
F0III-IVn: [HD13174, F0III-IVn]
F0IV: [HD27397, F0IV]
F0V: [HD108519, F0V(n)]
F1II: [HD173638_ext, F1II]
F1V: [HD213135, F1V]
F2-F5Ib: BD+38_2803, F2-F5Ib
F2Ib: [HD182835_ext, F2Ib]
F2III: [HD40535, F2III-IV]
F2V: [HD113139, F2V]
F3V: [HD26015, F3V]
F4III: [HD21770, F4III]
F4V: [HD16232, F4V]
F5.5III: [HD75555, F5.5III-IV]
F5Ib-G1Ib: [HD213306_ext, F5Ib-G1Ib]
F5III: [HD17918, F5III]
F5II-III: [HD186155, F5II-III]
F5V: [HD218804, F5V]
F6III-IV: [HD160365, F6III-IV]
F6IV: [HD11443, F6IV]
F6V: [HD215648, F6V]
F7II: [HD201078, F7II-]
F7III: [HD124850, F7III]
F7V: [HD126660, F7V]
F8.5IV-V: [HD102870, F8.5IV-V]
F8Ia: [HD190323_ext, F8Ia]
F8Ib: [HD51956_ext, F8Ib]
F8III: [HD220657, F8III]
F8IV: [HD111844, F8IV]
F8V: [HD219623, F8V]
F9.5V: [HD114710, F9.5V]
F9IIIa: [HD6903_ext, F9IIIa]
F9V: [HD176051, F9V]
wF9V: [HD165908, metalweak wF9V]
G0Ib-II: [HD185018_ext, G0Ib-II]
G0V: [HD109358, G0V]
G1.5V: [HD20619, G1.5V]
G1Ib: [HD74395, G1Ib]
G1III: [HD21018_ext, G1IIICH-1]
G1II: [HD216219, G1II-IIIFe-1CH0]
G1-V: [HD95128, G1-VFe-0.5]
G1V: [HD10307, G1V]
G2Ib: [HD39949_ext, G2Ib]
G2Ib: [HD3421, G2Ib-II]
G2II: [HD219477, G2II-III]
G2IV: [HD126868, G2IV]
G2V: [HD76151, G2V]
G3Ib-II: [HD192713_ext, G3Ib-IIWkH&Kcomp]
G3II: [HD176123_ext, G3II]
G3IIIb: [HD88639, G3IIIbFe-1]
G3Va: [HD10697, G3Va]
G4Ia: [HD6474_ext, G4Ia]
G4III: [HD108477, G4III]
G4O-Ia: [HD179821_ext, G4O-Ia]
G4V: [HD214850, G4V]
G5Ib: [HD190113_ext, G5Ib]
G5IIIa: [HD193896, G5IIIa]
G5IIICN: [HD18474., G5IIICN-3CH-2H]
G5V: [HD165185, G5V]
G6.5V: [HD115617, G6.5V]
G6IbH: [delta1_HD161664_ext, G6IbH]
G6Ib-IIa: [HD202314_ext, G6Ib-IIaCa1Ba0.5]
G6IIb: [HD58367, G6IIb]
G6III: [HD27277, G6III]
G7.5IIIa: [HD16139_ext, G7.5IIIa]
G7Ia: [HD333385_ext, G7Ia]
G7II: [HD25877_ext, G7II]
G7IIIa: [HD182694, G7IIIa]
G7IV: [HD114946, G7IV]
G7IV: [HD20618, G7IV]
G8Ib: [HD208606_ext, G8Ib]
G8IIIBa1: [HD104979, G8IIIBa1CN-1CH1]
G8IIIFe-1: [HD135722, G8IIIFe-1]
G8IIIFe-5: [HD122563, G8IIIFe-5]
G8V: [HD101501, G8V]
G9IICN1H: [delta1_HD170820_ext, G9IICN1H]
G9III: [HD222093, G9III]
K0.5IIb: [HD164349_ext, K0.5IIb]
K0.5IIICN1: [HD9852_ext, K0.5IIICN1]
K0Ia: [HD165782_ext, K0Ia]
K0Ib: [HD44391_ext, K0Ib]
K0II: [HD179870_ext, K0II]
K0III: [HD100006, K0III]
K0V: [HD145675, K0V]
K1.5IIIlines: [HD124897_lines_ext, K1.5IIIFe-0.5]
K1.5IIIflux: [HD124897_shape_ext, K1.5IIIFe-0.5]
K1Ia-Iab: [HD63302_ext, K1Ia-Iab]
K1-IIIb1: [HD91810, K1-IIIbCN1.5Ca1]
K1-IIIFe: [HD36134, K1-IIIFe-0.5]
K1III: [HD25975, K1III]
K1IVa: [HD142091, K1IVa]
K1IV: [HD165438, K1IV]
K1V: [HD10476, K1V]
K2.5II: [HD23082_ext, K2.5II]
K2IIIFe: [HD2901, K2IIIFe-1]
K2III: [HD132935_ext, K2III]
K2O-Ia: [HD212466_ext, K2O-Ia]
K2V: [HD3765, K2V]
K3.5IIIb: [HD114960, K3.5IIIbCN0.5CH0.5]
K3Iab-Ib: [HD187238_ext, K3Iab-Ib]
K3+IIIFe05: [HD99998_ext, K3+IIIFe-0.5]
K3IIIFe1: [HD35620_ext, K3IIIFe1]
K3III: [HD178208_ext, K3III]
K3II-III: [HD16068_ext, K3II-III]
K3V: [HD219134, K3V]
K4Ib: [HD185622A_ext, K4Ib]
K4Ib-II: [HD201065_ext, K4Ib-II]
K4-III: [HD207991_ext, K4-III]
K4V: [HD45977_ext, K4V]
K5.5III: [HD120477, K5.5III]
K5Ib: [HD216946_ext, K5Ib]
K5III: [HD181596, K5III]
K5V: [HD36003, K5V]
K6IIIa: [HD3346, K6IIIa]
K7IIa: [HD181475_ext, K7IIa]
K7III: [HD194193, K7III]
K7V: [HD201092, K7V]
kA9hF2mF2: [HD164136, kA9hF2mF2(IV)]
L0.5: [2MASSJ0746+2000AB, L0.5]
L1: [2MASSJ0208+2542, L1]
L2: [Kelu-1AB, L2]
L3: [2MASSJ1146+2230AB, L3]
L3.5: [2MASSJ0036+1821, L3.5]
L4.5: [2MASSJ2224-0158, L4.5]
L5: [2MASSJ1507-1627, L5]
L6: [2MASSJ1515+4847, L6(NIR)]
L7.5: [2MASSJ0825+2115, L7.5]
L8: [DENISJ0255-4700, L8]
M0.5Ib: [HD236697_ext, M0.5Ib]
M0.5V: [HD209290, M0.5V]
M0IIIb: [HD213893, M0IIIb]
M0V: [HD19305, M0V]
M10+III: [IRAS14086-0703, M10+III]
M1.5Iab-Ib: [HD35601_ext, M1.5Iab-Ib]
M1.5Ib: [BD+60_265_ext, M1.5Ib]
M1.5V: [HD36395, M1.5V]
M1-Iab-Ib: [HD14404_ext, M1-Iab-Ib]
M1Ia: [HD339034_ext, M1Ia]
M1+III: [HD204724, M1+III]
M1-M2Ia-Iab: [HD39801_ext, M1-M2Ia-Iab]
M1V: [HD42581, M1V]
M2.5IIIBa0.5: [HD219734, M2.5IIIBa0.5]
M2.5V: [Gl381, M2.5V]
M2-Ia: [HD206936_ext, M2-Ia]
M2Ib: [HD10465_ext, M2Ib]
M2II: [HD23475_ext, M2II]
M2III: [HD120052, M2III]
M2V: [Gl806, M2V]
M3.5I: [HD14488_ext, M3.5IabFe-1var]
M3.5III: [HD28487_ext, M3.5IIICa-0.5]
M3.5V: [Gl273, M3.5V]
M3Iab-Ia: [CD-31_49_ext, M3Iab-Ia]
M3IIb: [HD40239, M3IIb]
M3III: [HD39045_ext, M3III]
M3-M4Iab: [HD14469_ext, M3-M4Iab]
M3toM4: [RW_Cyg_ext, M3toM4Ia-Iab]
M3V: [Gl388, M3V]
M4.5IIIa: [HD204585, M4.5IIIa]
M4.5V: [Gl268AB, M4.5V]
M4+IIIa: [HD19058, M4+IIIa]
M4+III: [HD214665, M4+III]
M4III: [HD4408, M4III]
M4V: [Gl299_ext, M4V]
M5.5III: [HD94705, M5.5III]
M5e-M9eIII: [HD14386, M5e-M9eIII]
M5Ib-II: [HD156014, M5Ib-II]
M5III: [HD175865, M5III]
M5V: Gl866ABC_ext, M5V
M6.5StoM7: [HD142143, M6.5StoM7SIII]
M6.5V: [GJ1111, M6.5V]
M6e-M9eIII: [HD69243, M6e-M9eIII]
M6-III: [HD18191, M6-III]
M6III: [HD196610, M6III]
M6V: [Gl406, M6V]
M7-8III: [BRIB2339-0447, M7-8III]
M7-III: [HD108849, M7-III]
M7-M7.5I: [MY_Cep, M7-M7.5I]
M7V: [Gl644C, M7V]
M8-9III: [IRAS14303-1042, M8-9III]
M8III: [IRAS01037+1219, M8III]
M8V: [Gl752B, M8V]
M9.5V: [BRIB0021-0214, M9.5V]
M9III: [BRIB1219-1336, M9III]
M9V: [DENIS-PJ1048-3956, M9V]
Jupiter: [Jupiter, planet]
Neptune: [Neptune, planet]
Saturn: [Saturn, planet]
Uranus: [Uranus, planet]
S2.5Zr2: [BD+44_2267, S2.5Zr2]
S4.5Zr2Ti4: [HD64332, S4.5Zr2Ti4]
S5-S6Zr3: [HD62164, S5-S6Zr3to4Ti0]
SC5.5Zr: [HD44544, SC5.5Zr0.5]
T2: [SDSSJ1254-0122, T2]
T4.5: [2MASSJ0559-1404, T4.5]
AGN templates#
name: agn
type: agn
title: The AGN Atlas
abstract: |
This atlas contains a few spectral templates of AGNs covering the
ultraviolet to near-infrared spectral range (see Table 1 for spectral
coverage). The LINER and Seyfert 2 templates have been obtained with the
large aperture (10" by 20") and low resolution spectrographs of the IUE
satellite. The optical spectra were obtained through a long slit with a 10"
width, were a window of 20" long was extracted to mach the IUE aperture
(Calzetti 1995, private comm.). The flux of the LINER and Seyfert2 templates
is normalized to a Johnson visual magnitude of 12.5 (STMAG).
The Seyfert1 template consists of an UV spectrum obtained with the IUE low
resolution spectrographs and of a ground-based optical spectrum. The bright
QSO template is a composite spectrum from the Large Bright Quasar Survey
of Francie and collaborators (1991). The Seyfert1 and QSO spectral
templates are normalized to a Johnson blue magnitude of 12.5 (STMAG).
The NGC 1068 template is a composite spectrum. The continuum contains the
nebular, stellar, and power-law contributions. The observed fluxes and FWHM
of the UV, optical and near-IR emission lines are also incorporated into the
template (J.R. Walsh, private comm; read also the header of the STSDAS binary
for further details).
Details about how each template has been constructed can be found in the header
of the STSDAS binary file, or in the references given above. The header can be
read using the tupar task of the IRAF ttools package. STSDAS files can also be
dumped into an ASCII formatted file using the tdump task of the IRAF ttools package.
reference: Francis et al. 1991, ApJ 373, 465.
url: ""
spectral_coverage:
- UV
- VIS
- NIR
parameters:
resolution: 10 # [??]
wave_col: WAVELENGTH
flux_col: FLUX
file_extension: .fits
items:
liner: spectrum of M81
ngc1068: model, lines + cont.
qso: average of various spectra
seyfert1: spectrum of NGC 5548
seyfert2: spectrum of NGC 5548
Emission line nebulae#
name: nebulae
type: nebular
title: The Galactic Emission Line Object Atlas
abstract: |
This atlas contains the model spectra of the Orion nebula, and of the
planetary nebula NGC 7009. The templates cover the wavelength range from
0.1 to 1.1 microns.
The continuum of the Orion's template contains the nebular contribution
plus a combination of Kurucz model atmospheres to simulated the stellar
contribution. The fluxes of the UV, optical and near-IR emission lines
from different sources are also incorporated into the template (J.R. Walsh,
private comm).
The continuum of the planetery nebula has a nebular component and a hot
stellar component simulated by an 80000K black body. The fluxes of the UV,
optical and near-IR emission lines, from different sources, are also
incorporated into the template (J.R. Walsh, private comm.).
Details about how each individual template has been constructed can be found
in the header of the STSDAS binary files. The header can be read using the
tupar task of the IRAF ttools package. Files can also be dump into an ASCII
formatted file using the tdump task of the IRAF ttools package.
reference: ""
url: ""
spectral_coverage:
- UV
- VIS
- NIR
parameters:
resolution: 10 # [??]
wave_col: WAVELENGTH
flux_col: FLUX
file_extension: .fits
items:
orion: Orion Nebula
pn: Generic Planetary Nebula
Galaxy SEDs from the UV to the Mid-IR#
name: brown
type: extragalactic
synthetic: False
title: An Atlas of Galaxy Spectral Energy Distributions from the Ultraviolet to the Mid-infrared
abstract: |
We present an atlas of 129 spectral energy distributions for nearby galaxies,
with wavelength coverage spanning from the ultraviolet to the mid-infrared.
Our atlas spans a broad range of galaxy types, including ellipticals, spirals,
merging galaxies, blue compact dwarfs, and luminous infrared galaxies. We have
combined ground-based optical drift-scan spectrophotometry with infrared
spectroscopy from Spitzer and Akari with gaps in spectral coverage being
filled using Multi-wavelength Analysis of Galaxy Physical Properties spectral
energy distribution models. The spectroscopy and models were normalized,
constrained, and verified with matched-aperture photometry measured from
Swift, Galaxy Evolution Explorer, Sloan Digital Sky Survey, Two Micron All Sky
Survey, Spitzer, and Wide-field Infrared Space Explorer images. The
availability of 26 photometric bands allowed us to identify and mitigate
systematic errors present in the data. Comparison of our spectral energy
distributions with other template libraries and the observed colors of
galaxies indicates that we have smaller systematic errors than existing
atlases, while spanning a broader range of galaxy types. Relative to the prior
literature, our atlas will provide improved K-corrections, photometric
redshifts, and star-formation rate calibrations.
reference: Brown et al. 2014
bibcode: "2014ApJS..212...18B"
adsurl: "https://ui.adsabs.harvard.edu/abs/2014ApJS..212...18B"
doi: "10.1088/0067-0049/212/2/18"
url: "https://archive.stsci.edu/hlsp/galsedatlas"
spectral_coverage:
- UV
- VIS
- NIR
- MIR
parameters:
resolution: 2.5 # [??], in vis
wave_unit: Angstrom
flux_unit: FLAM
wave_col: WAVELENGTH
flux_col: FLUX
file_extension: .dat
items: # Morphology, BPT; full at https://archive.stsci.edu/hlsps/galsedatlas/atlas/hlsp_galsedatlas_multi_multi_summary_multi_v1_cat.csv
Arp256N: [SB(s)c, SF]
Arp256S: [SB(s)b, SF]
NGC0337: [SBd, SF]
CGCG436-030: [Pec, SF]
NGC0474: [(R)SA(s)0, Passive]
NGC0520: [Pec, SF/AGN]
NGC0584: [E4, Passive]
NGC0628: [SAc, Passive]
NGC0660: [SB(s)a, SF/AGN]
IIIZw035: [Pec, SF/AGN]
NGC0695: [S0, SF]
NGC0750: [Pec, Passive]
NGC0855: [E, SF]
NGC1068: [(R)SA(rs)b, AGN]
Arp118: [Pec, SF/AGN]
NGC1144: [Pec, SF]
NGC1275: [Pec, Passive]
NGC1614: [SB(s)c, SF/AGN]
NGC2388: [Irr, SF]
NGC2403: [SABcd, Passive]
NGC2537: [SB(s)m, SF]
NGC2623: [Pec, AGN]
IRAS08572+3915: [Pec, SF/AGN]
UGC04881: [Pec, SF]
NGC2798: [SBa pec, SF/AGN]
UGCA166: [Irr, SF]
UGC05101: [Pec, AGN]
NGC3049: [SBab, SF]
NGC3079: [SB(s)c, SF/AGN]
UGCA208: [Pec, AGN]
NGC3190: [SAa pec, Passive]
NGC3198: [SBc, SF]
NGC3265: [E, SF]
Mrk33: [Im pec, SF]
NGC3310: [SAB(r)bc, SF]
NGC3351: [SBb, SF]
NGC3379: [E0, Passive]
UGCA219: [Sc, SF]
NGC3521: [SABbc, SF]
NGC3627: [SABb, SF/AGN]
IC0691: [Irr, SF]
NGC3690: [Pec, SF/AGN]
NGC3773: [SA0, SF]
Mrk1450: [Irr, SF]
UGC06665: [Sb, SF]
NGC3870: [S0, SF]
UM461: [Irr, SF]
UGC06850: [Irr, SF]
NGC3938: [SAc, Passive]
NGC4088: [SAB(rs)bc, SF]
NGC4125: [E6 pec, Passive]
NGC4138: [SA(r)0, SF/AGN]
NGC4168: [E, Passive]
NGC4194: [Pec, SF/AGN]
Haro06: [Irr, SF]
NGC4254: [SAc, SF]
NGC4321: [SABbc, SF]
NGC4365: [E, Passive]
NGC4387: [E, Passive]
NGC4385: [SB(rs)0, SF/AGN]
NGC4450: [SAab, AGN]
NGC4458: [E, Passive]
NGC4473: [E, Passive]
NGC4486: [E, Passive]
NGC4536: [SABbc, SF]
NGC4550: [E, Passive]
NGC4551: [E, Passive]
NGC4552: [E, Passive]
NGC4559: [SABcd, SF]
NGC4569: [SABab, AGN]
NGC4579: [SABb, AGN]
NGC4594: [SAa, Passive]
NGC4625: [SABm pec, SF]
NGC4621: [E, Passive]
NGC4631: [SBd, AGN]
NGC4660: [E, Passive]
NGC4670: [SB(s)0/a, SF]
NGC4676A: [Pec, AGN]
NGC4725: [SABab pec, Passive]
NGC4826: [SAab, SF/AGN]
NGC4860: [E, Passive]
NGC4889: [E4, Passive]
IC4051: [E, Passive]
NGC4926: [E, Passive]
NGC5033: [SAc, SF/AGN]
IC0860: [Sa, AGN]
UGC08335NW: [Pec, SF/AGN]
UGC08335SE: [Pec, SF/AGN]
NGC5055: [SAbc, Passive]
IC0883: [Pec, SF/AGN]
NGC5104: [Sa, SF/AGN]
NGC5194: [SABbc pec, SF/AGN]
NGC5195: [SB0 pec, SF/AGN]
NGC5256: [Pec, AGN]
NGC5257: [SAB(s)b, SF]
NGC5258: [SA(s)b, SF]
UGC08696: [Pec, AGN]
Mrk1490: [Sa, SF/AGN]
NGC5653: [(R)SA(rs)b, SF]
Mrk0475: [Irr, SF]
NGC5713: [SABbc pec, SF]
UGC09618S: [Sc, SF/AGN]
UGC09618: [Pec, SF/AGN]
UGC09618N: [Sb, SF]
NGC5866: [S0, Passive]
CGCG049-057: [Irr, SF/AGN]
NGC5953: [Sa, SF/AGN]
IC4553: [Pec, AGN]
UGCA410: [Irr, SF]
NGC5992: [SBb, SF]
NGC6052: [Pec, SF]
NGC6090: [Pec, SF]
NGC6240: [Pec, AGN]
IRAS17208-0014: [Pec, SF]
IIZw096: [Pec, SF]
NGC7331: [SAb, SF/AGN]
UGC12150: [SB0/a, SF/AGN]
CGCG453-062: [Sab, SF]
IC5298: [Pec, AGN]
NGC7585: [(R)SA(s)0, Passive]
NGC7591: [SBbc, SF]
NGC7592: [Pec, SF/AGN]
NGC7673: [(R)SAc, SF]
NGC7674: [SA(r)bc, Passive]
NGC7679: [SB0, SF/AGN]
Mrk0930: [Pec, SF]
NGC7714: [SB(s)b, SF/AGN]
NGC7771: [SB(s)a, SF]
Mrk0331: [Sa, SF/AGN]
Subset of Kurucz 1993 Models (subset)#
name: kurucz
type: stellar
title: The 1993 Kurucz Stellar Atmospheres Atlas (excerpt)
abstract: |
This is an excerpt of the Kurucz Stellar Atmospheres Atlas with stellar
parameters selected to match common types.
reference: Kurucz CD-ROM, Cambridge, MA; Smithsonian Astrophysical Observatory, c1993, December 4, 1993
url: "http://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/kurucz-1993-models"
spectral_coverage:
- UV
- VIS
- NIR
- MIR
parameters:
resolution: 20 # [??]
wave_col: WAVELENGTH
flux_col: FLUX
file_extension: .fits
items: # parameters
o3v: {T: 50000, m/H: 0, logg: 5.0}
o5v: {T: 44500, m/H: 0, logg: 5.0}
o6v: {T: 41000, m/H: 0, logg: 5.0}
o8v: {T: 35800, m/H: 0, logg: 4.5}
b0v: {T: 30000, m/H: 0, logg: 3.9}
b3v: {T: 18700, m/H: 0, logg: 3.94}
b5v: {T: 15400, m/H: 0, logg: 4.04}
b8v: {T: 11900, m/H: 0, logg: 4.04}
a0v: {T: 9520, m/H: 0, logg: 4.14}
a5v: {T: 8200, m/H: 0, logg: 4.29}
f0v: {T: 7200, m/H: 0, logg: 4.34}
f5v: {T: 6440, m/H: 0, logg: 4.34}
g0v: {T: 6030, m/H: 0, logg: 4.39}
g2v: {T: 5860, m/H: 0, logg: 4.4}
k0v: {T: 5250, m/H: 0, logg: 4.49}
k5v: {T: 4350, m/H: 0, logg: 4.54}
m0v: {T: 3850, m/H: 0, logg: 4.59}
m2v: {T: 3580, m/H: 0, logg: 4.64}
m5v: {T: 3500, m/H: 0, logg: 4.94}
b0iii: {T: 29000, m/H: 0, logg: 3.5}
b5iii: {T: 15000, m/H: 0, logg: 3.49}
g0iii: {T: 5850, m/H: 0, logg: 2.94}
g5iii: {T: 5150, m/H: 0, logg: 2.54}
k0iii: {T: 4750, m/H: 0, logg: 2.14}
k5iii: {T: 3950, m/H: 0, logg: 1.74}
m0iii: {T: 3800, m/H: 0, logg: 1.34}
o5i: {T: 40000, m/H: 0, logg: 4.5}
o6i: {T: 39000, m/H: 0, logg: 4.5}
o8i: {T: 34200, m/H: 0, logg: 4.0}
b0i: {T: 26000, m/H: 0, logg: 3.0}
b5i: {T: 13600, m/H: 0, logg: 2.5}
a0i: {T: 9730, m/H: 0, logg: 2.14}
a5i: {T: 8510, m/H: 0, logg: 2.04}
f0i: {T: 7700, m/H: 0, logg: 1.74}
f5i: {T: 6900, m/H: 0, logg: 1.44}
g0i: {T: 5550, m/H: 0, logg: 1.34}
g5i: {T: 4850, m/H: 0, logg: 1.14}
k0i: {T: 4420, m/H: 0, logg: 0.94}
k5i: {T: 3850, m/H: 0, logg: 0.0}
m0i: {T: 3650, m/H: 0, logg: 0.0}
m2i: {T: 3600, m/H: 0, logg: 0.0}
Supernova Legacy Survey#
name: sne
type: supernova
title: Supernova spectral library
abstract: |
A collection of supernova spectra obtained with the sncosmo
package https://sncosmo.readthedocs.io/en/v2.0.x/index.html.
Please see there for the appropiated references.
Spectra are normalized to the maximum flux.
Most spectra are only for phase 0, time of maximum brightness,
unless otherwise noted
reference: "http://sncosmo.github.io/"
url: "https://sncosmo.readthedocs.io/en/v2.0.x/about.html"
spectral_coverage:
- UV
- VIS
- NIR
parameters:
resolution: 5 # [??]
wave_unit: Angstrom
flux_unit: FLAM
wave_col: WAVELENGTH
flux_col: FLUX
file_extension: .dat
items:
sn1a: [SALT2-extended, SNIa, phase 0]
sn1b: [SN1b, s11-2005hl]
sn1c: [SNIc, s11-2006fo]
sn2l: [SNIIL, s11-2004hx]
sn2p: [SNIIP, s11-2005lc]
sn2n: [SNIIn, snana-2006ez]
hyper: [nugent hyper-SN, SNIb/c, phase 5]
pop3_3d: [whalen-z25g, PopIII, phase 3]
pop3_15d: [whalen-z15g, PopIII, phase 15]
Flux/Telluric standards with X-Shooter#
name : moehler
type: stellar
title: Flux calibration of medium-resolution spectra from 300 nm to 2500 nm
abstract: |
We will provide standard star reference data that allow users to derive
response curves from 300 nm to 2500 nm for spectroscopic data of medium to
high resolution, including those taken with echelle spectrographs. In
addition we describe a method to correct for moderate telluric absorption
without the need of observing telluric standard stars. As reference data for
the flux standard stars we use theoretical spectra derived from stellar model
atmospheres. We verify that they provide an appropriate description of the
observed standard star spectra by checking for residuals in line cores and
line overlap regions in the ratios of observed (X-shooter) spectra to model
spectra. The finally selected model spectra are then corrected for remaining
mismatches and photometrically calibrated using independent observations. The
correction of telluric absorption is performed with the help of telluric
model spectra. We provide new, finely sampled reference spectra without
telluric absorption for six southern flux standard stars that allow the users
to flux calibrate their data from 300 nm to 2500 nm, and a method to correct
for telluric absorption using atmospheric models.
reference: Moehler et al. 2014
bibcode: "2014A&A...568A...9M"
adsurl: "https://ui.adsabs.harvard.edu/abs/2014A&A...568A...9M"
doi: "10.1051/0004-6361/201423790"
url: ""
spectral_coverage:
- UV
- VIS
- NIR
parameters:
resolution: 0.1 # [nm]
# wave_unit: nm # TODO: double check with FITS header
# flux_unit: 10mW/m2/nm # TODO: double check with FITS header
wave_col: lambda
flux_col: flux
file_extension: .fits
items: # teff, logg, spectral_type
EG274: [25985, 7.96, DA]
Feige110: [45250, 5.80, sdO]
GD153: [40320, 7.93, DA]
GD71: [33590, 7.93, DA]
L97-3: [10917, 8.15, DC]
LTT3218: [9081, 7.71, DA]
LTT7987: [16147, 7.98, DA]
High-Resolution Spectra of Habitable Zone Planets (example)#
name: madden
type: planetary
title: High-Resolution Spectra of Habitable Zone Planets
abstract: |
Simulated high-resolution spectra of habitable planets covering a wide
parameter space are essential in training retrieval tools, optimizing
observing strategies, and interpreting upcoming observations. Ground-based
extremely large telescopes like ELT, GMT, and TMT; and future space-based
mission concepts like Origins, HabEx, and LUVOIR are designed to have the
capability of characterizing a variety of potentially habitable worlds. Some
of these telescopes will use high precision radial velocity techniques to
obtain the required high-resolution spectra (R~100,000) needed to characterize
potentially habitable exoplanets. Here we present a database of
high-resolution (0.01 cm−1) reflection and emission spectra for simulated
exoplanets with a wide range of surfaces, receiving similar irradiation as
Earth around 12 different host stars from F0 to K7.
reference: Madden and Kaltenegger 2020, MNRAS 495, 1
url: https://zenodo.org/record/3930900
spectral_coverage:
- VIS
- NIR
- MIR
parameters:
resolution: 1.56e-7 # [um]
# wave_unit: um # TODO: double check with FITS header
# flux_unit: W/m2/um # TODO: double check with FITS header
wave_col: wavelength
flux_col: flux
file_extension: .fits
items:
example: sample spectrum
# to be expanded...
BOSZ Stellar Atmosphere Grid (subset) - High Resolution#
name: bosz/hr
type: stellar
synthetic: True
title: BOSZ Stellar Atmosphere Grid (subset) - High Resolution
abstract: |
This is a subset of the large BOSZ Stellar Atmosphere Grid. The subset
has been extracted to match the Pickles stellar library in temperature and gravity,
however not all types are fully covered.
reference: Bohlin et al. 2017, 153, 234
bibref: ""
adsurl: ""
doi: ""
url: "https://archive.stsci.edu/prepds/bosz/"
spectral_coverage:
- UV
- VIS
- NIR
- MIR
parameters:
waverange: [1000 AA, 32 um]
resolution: 100000 # [??]
"M/H": 0.0
"C/H": 0.0
"alpha/H": 0.0
vmic: 2.0 # microturbulent velocity [km/s]
vrot: 0.0 # rotational broadening [km/s]
wave_col: wavelength
flux_col: flux
file_extension: .fits
items: # parameters
o8v: {T: 35000, logg: 4.00}
b0v: {T: 30000, logg: 4.00}
b3v: {T: 18500, logg: 4.00}
b5v: {T: 15500, logg: 4.00}
b8v: {T: 12000, logg: 4.00}
a0v: {T: 9500, logg: 4.00}
a5v: {T: 8250, logg: 4.50}
f0v: {T: 7250, logg: 4.50}
f5v: {T: 6500, logg: 4.50}
g0v: {T: 6000, logg: 4.50}
g2v: {T: 5750, logg: 4.50}
k0v: {T: 5250, logg: 4.50}
k5v: {T: 4250, logg: 4.50}
m0v: {T: 3750, logg: 4.50}
m2v: {T: 3500, logg: 4.40}
b0iii: {T: 29000, logg: 3.50}
b5iii: {T: 15000, logg: 3.50}
g0iii: {T: 5750, logg: 3.00}
g5iii: {T: 5250, logg: 2.50}
k0iii: {T: 4750, logg: 2.00}
k5iii: {T: 4000, logg: 1.50}
m0iii: {T: 3750, logg: 1.50}
b0i: {T: 26000, logg: 3.00}
a0i: {T: 9750, logg: 2.00}
a5i: {T: 8500, logg: 2.00}
f0i: {T: 7750, logg: 1.50}
f5i: {T: 7000, logg: 1.50}
g0i: {T: 5550, logg: 1.50}
g5i: {T: 4750, logg: 1.00}
k0i: {T: 4500, logg: 1.00}
k5i: {T: 3750, logg: 0.00}
m2i: {T: 3500, logg: 0.00}
BOSZ Stellar Atmosphere Grid (subset) - Medium Resolution#
name: bosz/mr
type: stellar
synthetic: True
title: BOSZ Stellar Atmosphere Grid (subset) - Medium Resolution
abstract: |
This is a subset of the large BOSZ Stellar Atmosphere Grid. The subset
has been extracted to match the Pickles stellar library in temperature and gravity,
however not all types are fully covered.
reference: Bohlin et al. 2017, 153, 234
bibref: ""
adsurl: ""
doi: ""
url: "https://archive.stsci.edu/prepds/bosz/"
spectral_coverage:
- UV
- VIS
- NIR
- MIR
parameters:
waverange: [1000 AA, 32 um]
resolution: 20000 # [??]
"M/H": 0.0
"C/H": 0.0
"alpha/H": 0.0
vmic: 2.0 # microturbulent velocity [km/s]
vrot: 0.0 # rotational broadening [km/s]
wave_col: wavelength
flux_col: flux
file_extension: .fits
items: # parameters
o8v: {T: 35000, logg: 4.00}
b0v: {T: 30000, logg: 4.00}
b3v: {T: 18500, logg: 4.00}
b5v: {T: 15500, logg: 4.00}
b8v: {T: 12000, logg: 4.00}
a0v: {T: 9500, logg: 4.00}
a5v: {T: 8250, logg: 4.50}
f0v: {T: 7250, logg: 4.50}
f5v: {T: 6500, logg: 4.50}
g0v: {T: 6000, logg: 4.50}
g2v: {T: 5750, logg: 4.50}
k0v: {T: 5250, logg: 4.50}
k5v: {T: 4250, logg: 4.50}
m0v: {T: 3750, logg: 4.50}
m2v: {T: 3500, logg: 4.40}
b0iii: {T: 29000, logg: 3.50}
b5iii: {T: 15000, logg: 3.50}
g0iii: {T: 5750, logg: 3.00}
g5iii: {T: 5250, logg: 2.50}
k0iii: {T: 4750, logg: 2.00}
k5iii: {T: 4000, logg: 1.50}
m0iii: {T: 3750, logg: 1.50}
b0i: {T: 26000, logg: 3.00}
a0i: {T: 9750, logg: 2.00}
a5i: {T: 8500, logg: 2.00}
f0i: {T: 7750, logg: 1.50}
f5i: {T: 7000, logg: 1.50}
g0i: {T: 5550, logg: 1.50}
g5i: {T: 4750, logg: 1.00}
k0i: {T: 4500, logg: 1.00}
k5i: {T: 3750, logg: 0.00}
m2i: {T: 3500, logg: 0.00}
BOSZ Stellar Atmosphere Grid (subset) - Low Resolution#
name: bosz/lr
type: stellar
synthetic: True
title: BOSZ Stellar Atmosphere Grid (subset) - Low Resolution
abstract: |
This is a subset of the large BOSZ Stellar Atmosphere Grid. The subset
has been extracted to match the Pickles stellar library in temperature and gravity,
however not all types are fully covered.
reference: Bohlin et al. 2017, 153, 234
bibref: ""
adsurl: ""
doi: ""
url: "https://archive.stsci.edu/prepds/bosz/"
spectral_coverage:
- UV
- VIS
- NIR
- MIR
parameters:
waverange: [1000 AA, 32 um]
resolution: 5000 # [??]
"M/H": 0.0
"C/H": 0.0
"alpha/H": 0.0
vmic: 2.0 # microturbulent velocity [km/s]
vrot: 0.0 # rotational broadening [km/s]
wave_col: wavelength
flux_col: flux
file_extension: .fits
items: # parameters
o8v: {T: 35000, logg: 4.00}
b0v: {T: 30000, logg: 4.00}
b3v: {T: 18500, logg: 4.00}
b5v: {T: 15500, logg: 4.00}
b8v: {T: 12000, logg: 4.00}
a0v: {T: 9500, logg: 4.00}
a5v: {T: 8250, logg: 4.50}
f0v: {T: 7250, logg: 4.50}
f5v: {T: 6500, logg: 4.50}
g0v: {T: 6000, logg: 4.50}
g2v: {T: 5750, logg: 4.50}
k0v: {T: 5250, logg: 4.50}
k5v: {T: 4250, logg: 4.50}
m0v: {T: 3750, logg: 4.50}
m2v: {T: 3500, logg: 4.40}
b0iii: {T: 29000, logg: 3.50}
b5iii: {T: 15000, logg: 3.50}
g0iii: {T: 5750, logg: 3.00}
g5iii: {T: 5250, logg: 2.50}
k0iii: {T: 4750, logg: 2.00}
k5iii: {T: 4000, logg: 1.50}
m0iii: {T: 3750, logg: 1.50}
b0i: {T: 26000, logg: 3.00}
a0i: {T: 9750, logg: 2.00}
a5i: {T: 8500, logg: 2.00}
f0i: {T: 7750, logg: 1.50}
f5i: {T: 7000, logg: 1.50}
g0i: {T: 5550, logg: 1.50}
g5i: {T: 4750, logg: 1.00}
k0i: {T: 4500, logg: 1.00}
k5i: {T: 3750, logg: 0.00}
m2i: {T: 3500, logg: 0.00}
Paranal Night Sky Spectra#
Additionally, the Paranal sky emission spectra is also included
name: sky
type: background
title: Paranal Night Sky Spectra
abstract: |
This spectra have been generated with skycalc_ipy, an python interface to the
ESO Skycalc, at different resolutions (vLR: R800, LR: R4000, MR: R20000,
HR: R100000) using standard parameters. Wavelength steps are logaritmic so
resolution remains constant. No instrumental background is included. No
scattered Moon light is included. Parameters used for running skycalc_ipy are
stored in the header of each table. Tables also include values for
transmission, but those are not used in spextra and are provided for
completeness. Values for emission are in photons s-1 cm-2 angstrom-1 arcsec-2.
reference: "https://www.eso.org/observing/etc/bin/gen/form?INS.MODE=swspectr+INS.NAME=SKYCALC"
url: "https://skycalc-ipy.readthedocs.io/en/latest/"
spectral_coverage:
- UV
- VIS
- NIR
- MIR
wave_col: wavelength
flux_col: flux
file_extension: .fits
items: # R
HR: 100000
MR: 20000
LR: 4000
vLR: 800