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Lecture Notes in Physics
Editorial Board
H. Araki
Research InstituteforMathematical Sciences
Kyoto University, Kitashirakawa
Sakyo, ku, Kyoto 606, Japan
E. Br6zin
Ecole Normale Sup6rieure, D6partement de Physique
24, rue Lhomond, F-75231 ParisCedex 05, France
J.Ehlers
Max-Planck, InstitutfiirPhysik und Astrophysik, Ins... |
1
Atomic and Molecular Data
for Space Astronomy: Needs
and Availability
Peter L. Smith I and Wolfgang L. Wiese 2
ABSTRACT Atomic and molecular spectroscopicdata are essentialfor
the analysisof astronomicalspectraand formodelling conditionsin
astronomical objectswhere photon-induced processesare important. In order to
a... |
2
The Hubble Space Telescope
ScientificProblems and
Laboratory Data Needs
Steven N. Shore 1
ABSTRACT
This review concentrateson observationsthat willbe performed with the
new generationof space ultravioletspectrographs, especiallythe Goddard
High Resolution Spectrograph on the Hubble Space Telescope. The broad
astrophy... |
11
spectrum at one exposure, in contrastto the GHRS which requiresmany
individualorder observationsto cover the fullrange of the echelle. The
spectrographiscurrentlydesigned with two types ofdetectors: multi-anode
microchannel array (MAMA) and charge-coupled devices (CCDs), each
optimized to one of two broad wavelength... |
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BD+75 325 G140L
0 ItII
1350 . 1,370 1390 1410 1430 1450
Wovelength (A)
FIGURE 2.1.GHRS low resolutionspectrum of the hot subdwarf BD+75°325.
Notice the numerous strongfinesformed in thishot, high surface8ravity, stella~
atmosphere.
intensityand yet not too... |
20
trum from a wide varietyofstars, representingone ofthe primary absorbers
in the surrounding smog. In fact, mainly because of the thermal regulation
provided by the hydrogen Balmer lines, especiallyHa, the
typicaltemperature of astrophysicalplasmas isabout 10000K so the singly ionized iron
peak elements (20< Z <28) a... |
25
and other symbiotics, for instance V1016 Cyg (Nussbaumer et al. 1981).
Again, the work of identifyingthe linesis hampered by the lack of
assignments of multipletsfor many of these species. Since recombination is
important for these objects, many of the unidentifiedlinesmay arisefrom
very highly excited species (Nuss... |
29
observed resonance transitionof C II AA1334, 1335/~. Accurate oscillator
and collisionstrengths are required to translaterelativelevelpopulations
intodensity and temperature conditionsfor these clouds. As statedearlier,
the currentlyavailableopticaland UV spectrographs are not always able
to resolve the intrinsiclin... |
3
Atomic Data Needed for Far
Ultraviolet Astronomy with
HUT and FUSE
Jeffrey L. Linsky I
ABSTRACT I will summarize the spectroscopiccapabilitiesof existing
and planned space experiments, including HUT and FUSE, thatwillobtain
spectraof astronomicalsources at wavelengths shorterthan Lyman-a. The
important atomic and mol... |
38
3.3.1 ACCURATE WAVELENGTHS AND ENERGY LEVELS
Accurate absolute wavelengths are needed, for example, to measure
downflow and wind expansion velocitiesin stars, particularlyin the late-type
stars for which the wind expansion velocitiesin the atmospheric layers
accessibleto FUV and EUV instruments and the downflow velo... |
4
Atomic Data Needed for
Analysis of EUV and X-Ray
Spectra
John C. Raymond I
ABSTRACT Given high resolutionX-ray spectra, one can derivethe
temperaturestructure, elemental abundances, density, and in some cases
heating or cooling rateof a hot astrophysicalplasma. The accuracy of various
atomic ratecoefficientslimitsthe... |
0
v
0
I
48
0
1
2
3
4
6.4 6.6 6.8 7 7.2 7.4 7.6
Log T
FIGURE 4.2. Fe XX concentrationsfrom Arnaud and Raymond
(solid),Arnaud and Rothenfiug (dashed) and the 1990 version of Raymond and Smith
(long-dashed).
4.6 OVERALL UNCERTAINTY
There is no single number describing the uncertaintiesin the predicted
intensitiesof allX-r... |
55
10000 ~ isthe conversionmade to airwavelengths. Ifvacuum data are used
forthe calibrationspectra, the observed spectraautomaticallywillbe in
vacuum wavelengths, and therewillbe no questionwhether the
correctconversion formula to airwas used. One by-product would be the avoidance of
systematic errors in QSO redshifts... |
60
Ni II: Severalresonance absorptionlineshave been
detectedininterstellarclouds (Fig.3) and in the spectraof quasi-stellarobjects. However, only
thelineat1752 .~has an experimentaltransitionprobability.
Cu II: The lineat 1359/~ occurs ininterstellarspectrabut the lifetimeof
the upper levelcalculatedby Theodosiou (1986... |
66
References
Aashamar, K.,and Luke, T.M. 1990, J.Phys.,B23, L733.
Allison, A.C., and Dalgarno, A. 1970,Atomic Data, 1,289.
Anders, E.,and Grevesse, N. 1989, Geochim. Cosmochim. Acta, 53, 197.
Ansbacher, W., Li, Y.,and Pinnington, E.H. 1989,Phys. Lett. A, 139,165.
Bi6mont, E., Froese Fischer, C., Godefroid, M., Vaeck, ... |
71
There are fourscientificinstrumentsmounted atthe Cassegrain focus, each
one occupying an 80° segment ofthetotalfieldofview. The 20 arcminute field
of view is divided into four equal sectors with a pyramidal mirror. Each
instrumentsimultaneouslyreceivesa 3 arcminute fieldofa differentpartofthe
sky. Inordertoview thes... |
75
Molecular Spectroscopy
ElectronicTransitions
Surprisinglymany molecules have electronictransitionsatinfraredwavelengths.
Molecular ions can recombine with electronsto make highlyexcitedRydberg
stateswhich can emit a cascade of infraredradiationas they cool. These
transitionsare the molecular analogs of hydrogen reco... |
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