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"]
{'ref': 'A 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',
'assef': 'Low-resolution spectral templates for AGN and galaxies',
'sky': 'Paranal sky background spectra',
'shapley': 'Rest-Frame Ultraviolet Spectra of z ∼ 3 Lyman Break Galaxies',
'etc/kinney': 'ESO ETC version of the Kinney-Calzetti Atlas',
'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',
'etc/pickles': 'ESO ETC subset of the Pickles stellar library'}
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#
# A library with reference stars
library_name : ref
type : stars
title : Reference library for objects
summary : |
This library collects few objects than an be used as reference for calculations
reference : see CALSPEC
link : https://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/calspec
spectral_coverage :
- uv
- vis
- nir
- mir
resolution : 10
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : WAVELENGTH
flux_column_name : FLUX
data_type: fits
file_extension: .fits
templates: # comments
vega : Vega spectrum, 900A to 300um
vegaLR : Vega LR spectrum, 1148A to 2.6um
sirius : Sirius spectrum, 900A to 300um
sun : Solar spectrum, 1195A to 2.7um
sunHR : Solar HR spectrum, 1500A to 300um
The Kinney-Calzetti Spectral Atlas of Galaxies#
# THE KINNEY-CALZETTI SPECTRAL ATLAS OF GALAXIES
library_name : kc96
type : galaxies
title : The Kinney-Calzetti Spectral Atlas of Galaxies
summary : |
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, A.L., Calzetti, D., Bohlin, R.C., McQuade, K., Storchi-Bergmann, T. & Schmitt, H.R. 1996, ApJ, 467, 38
link : "http://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/the-kinney-calzetti-spetral-atlas"
spectral_coverage :
- uv
- vis
resolution : 10
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : WAVELENGTH
flux_column_name : FLUX
data_type: fits
file_extension: .fits
templates: # comments
elliptical : null
bulge : null
s0 : null
sa : null
sb : null
sc : null
starb1 : starburst with E(B-V)<0.1
starb2 : starburst with 0.11<E(B-V)<0.21
starb3 : starburst with 0.25<E(B-V)<0.35
starb4 : starburst with 0.39<E(B-V)<0.50
starb5 : starburst with 0.51<E(B-V)<0.60
starb6 : starburst with 0.61<E(B-V)<0.70
Pickles Stellar Library#
# Pickles Stellar Spectral Flux Library
library_name : pickles
type : stars
title : Pickles Stellar Spectral Flux Library
summary : |
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
link : "https://www.eso.org/sci/facilities/paranal/decommissioned/isaac/tools/lib.html"
spectral_coverage :
- uv
- vis
- nir
resolution : 5
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : WAVELENGTH
flux_column_name : FLUX
data_type: fits
file_extension: .fits
templates: # comments
o5v : null
o8iii : null
o9v : null
b0i : null
b0v : null
b12iii : null
b1i : null
b1v : null
b2ii : null
b2iv : null
b3i : null
b3iii : null
b3v : null
b57v : null
b5i : null
b5ii : null
b5iii : null
b6iv : null
b8i : null
b8v : null
b9iii : null
b9v : null
a0i : null
a0iii : null
a0iv : null
a0v : null
a2i : null
a2v : null
a3iii : null
a3v : null
a47iv : null
a5iii : null
a5v : null
a7iii : null
a7v : null
f02iv : null
f0i : null
f0ii : null
f0iii : null
f0v : null
f2ii : null
f2iii : null
f2v : null
f5i : null
f5iii : null
f5iv : null
f5v : null
f6v : null
f8i : null
f8iv : null
f8v : null
rf6v : metal rich
rf8v : metal rich
wf5v : metal weak
wf8v : metal weak
g0i : null
g0iii : null
g0iv : null
g0v : null
g2i : null
g2iv : null
g2v : null
g5i : null
g5ii : null
g5iii : null
g5iv : null
g5v : null
g8i : null
g8iii : null
g8iv : null
g8v : null
rg0v : metal rich
rg5iii : metal rich
rg5v : metal rich
wg0v : metal weak
wg5iii : metal weak
wg5v : metal weak
wg8iii : metal weak
k01ii : null
k0iii : null
k0iv : null
k0v : null
k1iii : null
k1iv : null
k2i : null
k2iii : null
k2v : null
k34ii : null
k3i : null
k3iii : null
k3iv : null
k3v : null
k4i : null
k4iii : null
k4v : null
k5iii : null
k5v : null
k7v : null
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 : null
m0v : null
m1iii : null
m1v : null
m2.5v : null
m2i : null
m2iii : null
m2v : null
m3ii : null
m3iii : null
m3v : null
m4iii : null
m4v : null
m5iii : null
m5v : null
m6iii : null
m6v : null
m7iii : null
m8iii : null
m9iii : null
m10iii : null
SDSS galaxy composite spectra#
# T A High Resolution Atlas of Composite SDSS Galaxy Spectra
library_name : dobos
type : galaxies
title : A High Resolution Atlas of Composite SDSS Galaxy Spectra
summary : |
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 {Δλ = 1 Å), 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
link : "http://www.vo.elte.hu/compositeatlas/v1/Default.aspx"
spectral_coverage :
- uv
- vis
resolution : 1
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : lambda
flux_column_name : flux
data_type: ascii
file_extension: .dat
templates: # comments
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#
# The IRTF Spectral Library
library_name : irtf
type :
- stars
- brown dwarfs
- planets
title : The IRTF Spectral Library
summary : |
The IRTF Spectral Library is a collection of 0.8-5.0 μm mostly stellar spectra observed at a resolving power of R = λ/Δλ ~ 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, J.T., Cushing, M.C., & Vacca, W.D., 2009, ApJS, 185, 289
link : "http://irtfweb.ifa.hawaii.edu/~spex/IRTF_Spectral_Library/index.html"
spectral_coverage :
- nir
- mir
resolution : 0.0015 # um
wave_unit: um
flux_unit : W m-2 um-1
wave_column_name : WAVELENGTH
flux_column_name : FLUX
data_type: ascii
file_extension: .dat
templates: # comments: star name, spec 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
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 plnt
Neptune: Neptune plnt
Saturn: Saturn plnt
Uranus: Uranus plnt
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#
# THE AGN ATLAS
library_name : agn
type : agn
title : THE AGN ATLAS
summary : |
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.
link : TBD
spectral_coverage :
- uv
- vis
- nir
resolution : 10
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : WAVELENGTH
flux_column_name : FLUX
data_type: fits
file_extension: .fits
templates: # comments
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#
# Nebulae
library_name : nebulae
type : nebulae
title : THE GALACTIC EMISSION LINE OBJECT ATLAS
summary : |
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 : TBD
link : TBD
spectral_coverage :
- uv
- vis
- nir
resolution : 10
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : WAVELENGTH
flux_column_name : FLUX
data_type: fits
file_extension: .fits
templates: # comments
orion: Orion
pn: Planetary Nebula
Galaxy SEDs from the UV to the Mid-IR#
# An Atlas of Galaxy Spectral Energy Distributions from the Ultraviolet to the Mid-infrared
library_name : brown
type : Galaxies
title : An Atlas of Galaxy Spectral Energy Distributions from the Ultraviolet to the Mid-infrared
summary : |
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, ApJS 212, 18
link : "https://archive.stsci.edu/hlsp/galsedatlas"
spectral_coverage :
- uv
- vis
- nir
- mir
resolution : 2.5 # optical
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : WAVELENGTH
flux_column_name : FLUX
data_type: ascii
file_extension: .dat
templates: # comments
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 Passove
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 Passove
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 pecSF/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)#
# THE 1993 KURUCZ STELLAR ATMOSPHERES ATLAS
library_name : kurucz
type : stars
title : The 1993 Kurucz Stellar Atmospheres Atlas (excerpt)
summary : |
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
link : "http://www.stsci.edu/hst/instrumentation/reference-data-for-calibration-and-tools/astronomical-catalogs/kurucz-1993-models"
spectral_coverage :
- uv
- vis
- nir
- mir
resolution : 20
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : WAVELENGTH
flux_column_name : FLUX
data_type: fits
file_extension: .fits
templates: #comments
o3v: T=50000, M/H=0, log(g)=5.0
o5v: T=44500, M/H=0, log(g)=5.0
o6v: T=41000, M/H=0, log(g)=5.0
o8v: T=35800, M/H=0, log(g)=4.5
b0v: T=30000, M/H=0, log(g)=3.9
b3v: T=18700, M/H=0, log(g)=3.94
b5v: T=15400, M/H=0, log(g)=4.04
b8v: T=11900, M/H=0, log(g)=4.04
a0v: T=9520, M/H=0, log(g)=4.14
a5v: T=8200, M/H=0, log(g)=4.29
f0v: T=7200, M/H=0, log(g)=4.34
f5v: T=6440, M/H=0, log(g)=4.34
g0v: T=6030, M/H=0, log(g)=4.39
g2v: T=5860, M/H=0, log(g)=4.4
k0v: T=5250, M/H=0, log(g)=4.49
k5v: T=4350, M/H=0, log(g)=4.54
m0v: T=3850, M/H=0, log(g)=4.59
m2v: T=3580, M/H=0, log(g)=4.64
m5v: T=3500, M/H=0, log(g)=4.94
b0iii: T=29000, M/H=0, log(g)=3.5
b5iii: T=15000, M/H=0, log(g)=3.49
g0iii: T=5850, M/H=0, log(g)=2.94
g5iii: T=5150, M/H=0, log(g)=2.54
k0iii: T=4750, M/H=0, log(g)=2.14
k5iii: T=3950, M/H=0, log(g)=1.74
m0iii: T=3800, M/H=0, log(g)=1.34
o5i: T=40000, M/H=0, log(g)=4.5
o6i: T=39000, M/H=0, log(g)=4.5
o8i: T=34200, M/H=0, log(g)=4.0
boi: T=26000, M/H=0, log(g)=3.0
b5i: T=13600, M/H=0, log(g)=2.5
aoi: T=9730, M/H=0, log(g)=2.14
a5i: T=8510, M/H=0, log(g)=2.04
f0i: T=7700, M/H=0, log(g)=1.74
f5i: T=6900, M/H=0, log(g)=1.44
g0i: T=5550, M/H=0, log(g)=1.34
g5i: T=4850, M/H=0, log(g)=1.14
k0i: T=4420, M/H=0, log(g)=0.94
k5i: T=3850, M/H=0, log(g)=0.0
m0i: T=3650, M/H=0, log(g)=0.0
m2i: T=3600, M/H=0, log(g)=0.0
Supernova Legacy Survey#
# Supernova Spectra
library_name : sne
type : supernova
title : Supernova spectral library
summary : |
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/
link : https://sncosmo.readthedocs.io/en/v2.0.x/about.html
spectral_coverage :
- uv
- vis
- nir
resolution : 5
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : WAVELENGTH
flux_column_name : FLUX
data_type: ascii
file_extension: .dat
templates: # comments
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#
#
library_name : moehler
type : stars
title : Flux calibration of medium-resolution spectra from 300 nm to 2500 nm
summary : |
We will provide standard star reference data that allow users to derive response curves
from 300nm to 2500nm 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 300nm to 2500nm, and a
method to correct for telluric absorption using atmospheric models.
reference : Moehler et al. 2014, A&A 568, A9
link : TB
spectral_coverage :
- uv
- vis
- nir
resolution : 0.1
wave_unit: nm
flux_unit : 10mW/m2/nm
wave_column_name : lambda
flux_column_name : flux
data_type: fits
file_extension: .fits
templates: # comments
eg274 : EG274, Te=25985, logg=7.96, DA
feige110 : Feige110, Te=45250, logg=5.80, sdO
gd153 : GD153, Te=40320, logg=7.93, DA
gd71 : GD71, Te=33590, logg=7.93, DA
l97-3 : L97-3, Te=10917, logg=8.15, DC
ltt3218 : LTT3218, Te=9081, logg=7.71, DA
ltt7987 : LTT7987, Te=16147, logg=7.98, DA
High-Resolution Spectra of Habitable Zone Planets (example)#
#
library_name : madden
type : planets
title : High-Resolution Spectra of Habitable Zone Planets
summary : |
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
link : https://zenodo.org/record/3930900
spectral_coverage :
- vis
- nir
- mir
resolution : 1.56e-7
wave_unit: um
flux_unit : W/m2/um
wave_column_name : wavelength
flux_column_name : flux
data_type: fits
file_extension: .fits
templates: # comments
example : sample spectrum
BOSZ Stellar Atmosphere Grid (subset) - High Resolution#
# BOSZ STELLAR ATMOSPHERES GRID
library_name : bosz/hr
type : stars
title : BOSZ Stellar Atmosphere Grid (subset) - High Resolution
summary : |
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. This libary has the following parameters
Wavelength coverage = 1000A - 32um
Resolution = 100000
M/H = 0.0
C/H = 0.0
alpha/H = 0.0
Microturbulent velocity = 2.0 km/s
Rotational Broadening = 0.0 km/s
reference : Bohlin et al. 2017, 153, 234
link : "https://archive.stsci.edu/prepds/bosz/"
spectral_coverage :
- uv
- vis
- nir
- mir
resolution : 100000
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : wavelength
flux_column_name : flux
data_type: fits
file_extension: .fits
templates: # comments
o8v : T=35000, log(g)=4.00
b0v : T=30000, log(g)=4.00
b3v : T=18500, log(g)=4.00
b5v : T=15500, log(g)=4.00
b8v : T=12000, log(g)=4.00
a0v : T=9500, log(g)=4.00
a5v : T=8250, log(g)=4.50
f0v : T=7250, log(g)=4.50
f5v : T=6500, log(g)=4.50
g0v : T=6000, log(g)=4.50
g2v : T=5750, log(g)=4.50
k0v : T=5250, log(g)=4.50
k5v : T=4250, log(g)=4.50
m0v : T=3750, log(g)=4.50
m2v : T=3500, log(g)=4.40
b0iii : T=29000, log(g)=3.50
b5iii : T=15000, log(g)=3.50
g0iii : T=5750, log(g)=3.00
g5iii : T=5250, log(g)=2.50
k0iii : T=4750, log(g)=2.00
k5iii : T=4000, log(g)=1.50
m0iii : T=3750, log(g)=1.50
b0i : T=26000, log(g)=3.00
a0i : T=9750, log(g)=2.00
a5i : T=8500, log(g)=2.00
f0i : T=7750, log(g)=1.50
f5i : T=7000, log(g)=1.50
g0i : T=5550, log(g)=1.50
g5i : T=4750, log(g)=1.00
k0i : T=4500, log(g)=1.00
k5i : T=3750, log(g)=0.00
m2i : T=3500, log(g)=0.00
BOSZ Stellar Atmosphere Grid (subset) - Medium Resolution#
# BOSZ STELLAR ATMOSPHERES GRID
library_name : bosz/mr
type : stars
title : BOSZ Stellar Atmosphere Grid (subset) - Medium Resolution
summary : |
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. This libary has the following parameters
Wavelength coverage = 1000A - 32um
Resolution = 20000
M/H = 0.0
C/H = 0.0
alpha/H = 0.0
Microturbulent velocity = 2.0 km/s
Rotational Broadening = 0.0 km/s
reference : Bohlin et al. 2017, 153, 234
link : "https://archive.stsci.edu/prepds/bosz/"
spectral_coverage :
- uv
- vis
- nir
- mir
resolution : 20000
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : wavelength
flux_column_name : flux
data_type: fits
file_extension: .fits
templates: # comments
o8v : T=35000, log(g)=4.00
b0v : T=30000, log(g)=4.00
b3v : T=18500, log(g)=4.00
b5v : T=15500, log(g)=4.00
b8v : T=12000, log(g)=4.00
a0v : T=9500, log(g)=4.00
a5v : T=8250, log(g)=4.50
f0v : T=7250, log(g)=4.50
f5v : T=6500, log(g)=4.50
g0v : T=6000, log(g)=4.50
g2v : T=5750, log(g)=4.50
k0v : T=5250, log(g)=4.50
k5v : T=4250, log(g)=4.50
m0v : T=3750, log(g)=4.50
m2v : T=3500, log(g)=4.40
b0iii : T=29000, log(g)=3.50
b5iii : T=15000, log(g)=3.50
g0iii : T=5750, log(g)=3.00
g5iii : T=5250, log(g)=2.50
k0iii : T=4750, log(g)=2.00
k5iii : T=4000, log(g)=1.50
m0iii : T=3750, log(g)=1.50
b0i : T=26000, log(g)=3.00
a0i : T=9750, log(g)=2.00
a5i : T=8500, log(g)=2.00
f0i : T=7750, log(g)=1.50
f5i : T=7000, log(g)=1.50
g0i : T=5550, log(g)=1.50
g5i : T=4750, log(g)=1.00
k0i : T=4500, log(g)=1.00
k5i : T=3750, log(g)=0.00
m2i : T=3500, log(g)=0.00
BOSZ Stellar Atmosphere Grid (subset) - Low Resolution#
# BOSZ STELLAR ATMOSPHERES GRID
library_name : bosz/lr
type : stars
title : BOSZ Stellar Atmosphere Grid (subset) - Low Resolution
summary : |
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. This libary has the following parameters
Wavelength coverage = 1000A - 32um
Resolution = 5000
M/H = 0.0
C/H = 0.0
alpha/H = 0.0
Microturbulent velocity = 2.0 km/s
Rotational Broadening = 0.0 km/s
reference : Bohlin et al. 2017, 153, 234
link : "https://archive.stsci.edu/prepds/bosz/"
spectral_coverage :
- uv
- vis
- nir
- mir
resolution : 5000
wave_unit: Angstrom
flux_unit : FLAM
wave_column_name : wavelength
flux_column_name : flux
data_type: fits
file_extension: .fits
templates: # comments
o8v : T=35000, log(g)=4.00
b0v : T=30000, log(g)=4.00
b3v : T=18500, log(g)=4.00
b5v : T=15500, log(g)=4.00
b8v : T=12000, log(g)=4.00
a0v : T=9500, log(g)=4.00
a5v : T=8250, log(g)=4.50
f0v : T=7250, log(g)=4.50
f5v : T=6500, log(g)=4.50
g0v : T=6000, log(g)=4.50
g2v : T=5750, log(g)=4.50
k0v : T=5250, log(g)=4.50
k5v : T=4250, log(g)=4.50
m0v : T=3750, log(g)=4.50
m2v : T=3500, log(g)=4.40
b0iii : T=29000, log(g)=3.50
b5iii : T=15000, log(g)=3.50
g0iii : T=5750, log(g)=3.00
g5iii : T=5250, log(g)=2.50
k0iii : T=4750, log(g)=2.00
k5iii : T=4000, log(g)=1.50
m0iii : T=3750, log(g)=1.50
b0i : T=26000, log(g)=3.00
a0i : T=9750, log(g)=2.00
a5i : T=8500, log(g)=2.00
f0i : T=7750, log(g)=1.50
f5i : T=7000, log(g)=1.50
g0i : T=5550, log(g)=1.50
g5i : T=4750, log(g)=1.00
k0i : T=4500, log(g)=1.00
k5i : T=3750, log(g)=0.00
m2i : T=3500, log(g)=0.00
Paranal Night Sky Spectra#
Additionally, the Paranal sky emission spectra is also included
# Paranal Night Sky Spectra
library_name : sky
type : background
title : Paranal Night Sky Spectra
summary : |
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 so resolution remains constant.
Noinstrumental 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 aren't 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
link : https://skycalc-ipy.readthedocs.io/en/latest/
spectral_coverage :
- uv
- vis
- nir
- mir
resolution : 1
wave_unit: angstrom
flux_unit : photlam
wave_column_name : wavelength
flux_column_name : flux
data_type: fits
file_extension: .fits
templates: # comments
HR : High Resolution, R=100000
MR : Medium Resolution, R=20000
LR : Low Resolution, R=4000
vLR : very Low Resolution, R=800