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FUSE Measurements of Far-Ultraviolet Extinction. III. The Dependence on R(V) and Discrete Feature Limits from 75 Galactic Sightlines
We present a sample of 75 extinction curves derived from Far UltravioletSpectroscopic Explorer (FUSE) far-ultraviolet spectra supplemented byexisting International Ultraviolet Explorer (IUE) spectra. Theextinction curves were created using the standard pair method based on anew set of dereddened FUSE+IUE comparison stars. Molecular hydrogenabsorption features were removed using individualized H2models for each sightline. The general shape of the FUSE extinction (8.4μm-1 < λ-1 < 11μm-1) was found to be broadly consistent withextrapolations from the IUE extinction (3.3 μm-1< λ-1 < 8.6 μm-1)curve. Significant differences were seen in the strength of the far-UVrise and the width of the 2175 Å bump. All the FUSE+IUE extinctioncurves had positive far-UV slopes giving no indication that the far-UVrise was turning over at the shortest wavelengths. The dependence ofA(λ)/A(V) versus R(V)-1 in the far-UV using thesightlines in our sample was found to be stronger than tentativelyindicated by previous work. We present an updated R(V)-dependentrelationship for the full UV wavelength range (3.3μm-1 <= λ-1 <= 11μm-1). Finally, we searched for discrete absorptionfeatures in the far-ultraviolet. We found a 3σ upper limit of~0.12A(V) on features with a resolution of 250 (~4 Å width) and3σ upper limits of ~0.15A(V) for λ-1 <9.6 μm-1 and ~0.68A(V) forλ-1>9.6 μm-1 on featureswith a resolution of 104 (~0.1 Å width).
| A Unified Representation of Gas-Phase Element Depletions in the Interstellar Medium
A study of gas-phase element abundances reported in the literature for17 different elements sampled over 243 sight lines in the local part ofour Galaxy reveals that the depletions into solid form (dust grains) areextremely well characterized by trends that employ only three kinds ofparameters. One is an index that describes the overall level ofdepletion applicable to the gas in any particular sight line, and theother two represent linear coefficients that describe how to derive eachelement's depletion from this sight-line parameter. The information fromthis study reveals the relative proportions of different elements thatare incorporated into dust at different stages of grain growth. Anextremely simple scheme is proposed for deriving the dust contents andmetallicities of absorption-line systems that are seen in the spectra ofdistant quasars or the optical afterglows of gamma-ray bursts. Contraryto presently accepted thinking, the elements sulfur and krypton appearto show measurable changes in their depletions as the general levels ofdepletions of other elements increase, although more data are needed toascertain whether or not these findings are truly compelling. Nitrogenappears to show no such increase. The incorporation of oxygen into solidform in the densest gas regions far exceeds the amounts that can takethe form of silicates or metallic oxides; this conclusion is based ondifferential measurements of depletion and thus is unaffected byuncertainties in the solar abundance reference scale.Based in large part on published observations from (1) the NASA/ESAHubble Space Telescope obtained at the Space Telescope ScienceInstitute, which is operated by the Association of Universities forResearch in Astronomy, Inc., under NASA contract NAS 5-26555, (2) theFar Ultraviolet Spectroscopic Explorer (FUSE) mission operated by JohnsHopkins University, supported by NASA contract NAS5-32985, and (3) TheCopernicus satellite, supported by NASA grant NAGW-77 to PrincetonUniversity.
| Pulkovo compilation of radial velocities for 35495 stars in a common system.
Not Available
| An Extended FUSE Survey of Diffuse O VI Emission in the Interstellar Medium
We present a survey of diffuse O VI emission in the interstellar medium(ISM) obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE).Spanning 5.5 yr of FUSE observations, from launch through 2004 December,our data set consists of 2925 exposures along 183 sight lines, includingall of those with previously published O VI detections. The data wereprocessed using an implementation of CalFUSE version 3.1 modified tooptimize the signal-to-noise ratio and velocity scale of spectra from anaperture-filling source. Of our 183 sight lines, 73 show O VIλ1032 emission, 29 at >3 σ significance. Six of the 3σ features have velocities |vLSR|>120 kms-1, while the others have |vLSR|<=50 kms-1. Measured intensities range from 1800 to 9100 LU (lineunit; 1 photon cm-2 s-1 sr-1), with amedian of 3300 LU. Combining our results with published O VI absorptiondata, we find that an O VI-bearing interface in the local ISM yields anelectron density ne=0.2-0.3 cm-3 and a path lengthof 0.1 pc, while O VI-emitting regions associated with high-velocityclouds in the Galactic halo have densities an order of magnitude lowerand path lengths 2 orders of magnitude longer. Although the O VIintensities along these sight lines are similar, the emission isproduced by gas with very different properties.Based on observations made with the NASA-CNES-CSA Far UltravioletSpectroscopic Explorer. FUSE is operated for NASA by Johns HopkinsUniversity under NASA contract NAS5-32985.
| X-Ray Absorption Spectroscopy of the Multiphase Interstellar Medium: Oxygen and Neon Abundances
X-ray absorption spectroscopy provides a powerful tool in determiningthe metal abundances in various phases of the interstellar medium (ISM).We present a case study of the sight line toward 4U 1820-303, based onChandra grating observations. The detection of O I, O II, O III, O VII,O VIII, and Ne IX Kα absorption lines allows us to measure theatomic column densities of the neutral, warm ionized, and hot phases ofthe ISM through much of the Galactic disk. By comparing thesemeasurements with the 21 cm hydrogen emission and with the pulsardispersion measure, we estimate the mean oxygen abundances in theneutral and total ionized phases as 0.3(0.2, 0.6) and 2.2(1.1, 3.5) inunits of Anders & Greversse's solar value (90% confidenceintervals). This significant oxygen abundance difference is apparently aresult of molecule/dust grain destruction and recent metal enrichment inthe warm ionized and hot phases. We also measure the column density ofneon from its absorption edge and obtain a solar value of the Ne/O ratioaccounting for the expected oxygen contained in molecules and dustgrains. From a joint analysis of the O VII, O VIII, and Ne IX lines, weobtain the Ne/O abundance ratio of the hot phase as 1.4(0.9, 2.1) solar,which is not sensitive to the exact hot gas temperature distributionassumed. These comparable ISM Ne/O ratios for the different phases arethus considerably less than the value recently inferred from coronaemission of solar-like stars.
| New Estimates of the Solar-Neighborhood Massive Star Birthrate and the Galactic Supernova Rate
The birthrate of stars of masses >=10 Msolar is estimatedfrom a sample of just over 400 O3-B2 dwarfs within 1.5 kpc of the Sunand the result extrapolated to estimate the Galactic supernova ratecontributed by such stars. The solar-neighborhood Galactic-plane massivestar birthrate is estimated at ~176 stars kpc-3Myr-1. On the basis of a model in which the Galactic stellardensity distribution comprises a ``disk+central hole'' like that of thedust infrared emission (as proposed by Drimmel and Spergel), theGalactic supernova rate is estimated at probably not less than ~1 normore than ~2 per century and the number of O3-B2 dwarfs within the solarcircle at ~200,000.
| Observations of the Diffuse Far-Ultraviolet Background with the Far Ultraviolet Spectroscopic Explorer
We have used observations taken under the Far Ultraviolet SpectroscopicExplorer (FUSE) S405/505 channel realignment program to explore thediffuse far-ultraviolet (FUV; 1000-1200 Å) radiation field. Of the71 independent locations in that program, we have observed a diffusesignal in 32, ranging in brightness from 1600 to a maximum of2.9×105 photons cm-2 sr-1s-1 Å-1 in Orion. The FUSE data confirm thatthe diffuse FUV sky is patchy with regions of intense emission, usuallynear bright stars, but also with dark regions, even at low Galacticlatitudes. We find a weak correlation between the FUV flux and the 100μm ratio but with wide variations, perhaps due to differences in thelocal radiation field.Based on observations made with the NASA-CNES-CSA Far UltravioletSpectroscopic Explorer. FUSE is operated for NASA by The Johns HopkinsUniversity under NASA contract NAS5-32985.
| Catalog of Galactic OB Stars
An all-sky catalog of Galactic OB stars has been created by extendingthe Case-Hamburg Galactic plane luminous-stars surveys to include 5500additional objects drawn from the literature. This work brings the totalnumber of known or reasonably suspected OB stars to over 16,000.Companion databases of UBVβ photometry and MK classifications forthese objects include nearly 30,000 and 20,000 entries, respectively.
| Highly Ionized Gas in the Galactic Halo: A FUSE Survey of O VI Absorption toward 22 Halo Stars
Far Ultraviolet Spectroscopic Explorer (FUSE) spectra of 22 Galactichalo stars are studied to determine the amount of O VI in the Galactichalo between ~0.3 and ~10 kpc from the Galactic midplane. Strong O VIλ1031.93 absorption was detected toward 21 stars, and a reliable3 σ upper limit was obtained toward HD 97991. The weaker member ofthe O VI doublet at 1037.62 Å could be studied toward only sixstars because of stellar and interstellar blending problems. Themeasured logarithmic total column densities vary from 13.65 to 14.57with =14.17+/-0.28 (1 σ). The observed columns arereasonably consistent with a patchy exponential O VI distribution with amidplane density of 1.7×10-8 cm-3 and scaleheight between 2.3 and 4 kpc. We do not see clear signs of stronghigh-velocity components in O VI absorption along the Galactic sightlines, which indicates the general absence of high-velocity O VI within2-5 kpc of the Galactic midplane. This result is in marked contrast tothe findings of Sembach et al., who reported high-velocity O VIabsorption toward ~60% of the complete halo sight lines observed byFUSE. The line centroid velocities of the O VI absorption do not reflectGalactic rotation well. The O VI velocity dispersions range from 33 to78 km s-1, with an average of =45+/-11 kms-1 (1 σ). These values are much higher than the valueof ~18 km s-1 expected from thermal broadening for gas atT~3×105 K, the temperature at which O VI is expected toreach its peak abundance in collisional ionization equilibrium.Turbulence, inflow, and outflow must have an effect on the shape of theO VI profiles. Kinematical comparisons of O VI with Ar I reveal thateight of 21 sight lines are closely aligned in LSR velocity(|ΔVLSR|<=5 km s-1), while nine of 21exhibit significant velocity differences(|ΔVLSR|>=15 km s-1). This dual behaviormay indicate the presence of two different types of O VI-bearingenvironments toward the Galactic sight lines. The correlation betweenthe H I and O VI intermediate-velocity absorption is poor. We couldidentify the known H I intermediate-velocity components in the Ar Iabsorption but not in the O VI absorption in most cases. Comparison of OVI with other highly ionized species suggests that the high ions areproduced primarily by cooling hot gas in the Galactic fountain flow andthat turbulent mixing also has a significant contribution. The role ofturbulent mixing varies from negligible to dominant. It is mostimportant toward sight lines that sample supernova remnants like Loops Iand IV. The average N(C IV)/N(O VI) ratios for the nearby halo (thiswork) and complete halo (Savage et al.) are similar (~0.6), but thedispersion is larger in the sample of nearby halo sight lines. We areable to show that the O VI enhancement toward the Galactic center regionthat was observed in the FUSE survey of complete halo sight lines(Savage et al.) is likely associated with processes occurring near theGalactic center by comparing the observations toward the nearby HD177566 sight line to those toward extragalactic targets.
| Synthetic High-Resolution Line Spectra of Star-forming Galaxies below 1200 Å
We have generated a set of far-ultraviolet stellar libraries usingspectra of OB and Wolf-Rayet stars in the Galaxy and the Large and SmallMagellanic Cloud. The spectra were collected with the Far UltravioletSpectroscopic Explorer and cover a wavelength range from 1003.1 to1182.7 Å at a resolution of 0.127 Å. The libraries extendfrom the earliest O to late-O and early-B stars for the Magellanic Cloudand Galactic libraries, respectively. Attention is paid to the complexblending of stellar and interstellar lines, which can be significant,especially in models using Galactic stars. The most severe contaminationis due to molecular hydrogen. Using a simple model for the H2line strength, we were able to remove the molecular hydrogen lines in asubset of Magellanic Cloud stars. Variations of the photospheric andwind features of C III λ1176, O VI λλ1032, 1038, PV λλ1118, 1128, and S IV λλ1063, 1073, 1074are discussed as a function of temperature and luminosity class. Thespectral libraries were implemented into the LavalSB and Starburst99packages and used to compute a standard set of synthetic spectra ofstar-forming galaxies. Representative spectra are presented for variousinitial mass functions and star formation histories. The valid parameterspace is confined to the youngest ages of less than ~=10 Myr for aninstantaneous burst, prior to the age when incompleteness of spectraltypes in the libraries sets in. For a continuous burst at solarmetallicity, the parameter space is not limited. The suite of models isuseful for interpreting the rest-frame far-ultraviolet in local andhigh-redshift galaxies. Based on observations made with theNASA-CNES-CSA Far Ultraviolet Spectroscopic Explorer. FUSE is operatedfor NASA by the Johns Hopkins University under NASA contract NAS5-32985.
| The total-to-selective extinction ratio determined from near IR photometry of OB stars
The paper presents an extensive list of the total to selectiveextinction ratios R calculated from the infrared magnitudes of 597 O andB stars using the extrapolation method. The IR magnitudes of these starswere taken from the literature. The IR colour excesses are determinedwith the aid of "artificial standards" - Wegner (1994). The individualand mean values of total to selective extinction ratios R differ in mostcases from the average value R=3.10 +/-0.05 - Wegner (1993) in differentOB associations. The relation between total to selective extinctionratios R determined in this paper and those calculated using the "methodof variable extinction" and the Cardelli et al. (1989) formulae isdiscussed. The R values presented in this paper can be used to determineindividual absolute magnitudes of reddened OB stars with knowntrigonometric parallaxes.
| A study of the behaviour of the NaI/KI column density ratio in the interstellar medium using the Na ultraviolet doublet
Here we make a new study of the behaviour of the NaI/KI column densityratio in the interstellar medium, using a sample of new observations of28 stars obtained at the Nordic Optical Telescope (NOT) in 1996 and1997, and previously published observations (obtained by some of theauthors) of 21 stars. The sightlines cover a range of distances anddirections, including into the Galactic halo. We make use of newobservations of the NaI ultraviolet (UV) doublet for some 18 stars. Thisdoublet is much weaker than the NaI D doublet and so is less susceptibleto saturation effects, and it is well known that it can be used toobtain more accurate NaI column densities with a smaller error range. Wefind an average N(NaI)/N(KI) ratio from the NaI UV data of about 90,which is rather higher than that found previously by Hobbs and Lequeux.The Na UV-KI ratio shows a small increase in value with increasingcolumn density, while we also find a sample of low N(NaI)/N(KI) ratioclouds generally seen towards distant objects on high-latitudesightlines that reach into the halo, so that the ratio decreases moresharply at lower column densities. As the values of the ratio for thesehalo clouds (10-20) bracket the cosmic Na/K abundance ratio, we suggestthat these ratios result from a harder radiation field in the lowerhalo, such that the ionized fractions of NaI and KI become similar.Clearly caution needs to be applied in using any kind of `standardvalue' for the NaI/KI column density ratio.
| Atlas of Interstellar Extinction Curves of OB Stars Covering the Whole Available Wavelength Range
The paper presents a collection of 436 extinction curves covering thewhole available range of wavelengths from satellite UV to near-IR. Thedata were taken from the ANS photometric catalogue and from thecompilations of IR photometric measurements. The data curves have beenobtained with the aid of ``artificial standards": Papaj et al. (1993)and Wegner (1994, 1995). The visual magnitudes and spectralclassifications of O and B type stars with EB-V>= 0.05were taken from the SIMBAD database. The curves are given in the form ofplots and tables E{lambda - V} / EB-V versus1/λ. The observed variety of extinction laws among slightlyreddened stars is apparently due to the various physical parameters ofinterstellar clouds.
| 900-1200 Å Interstellar Extinction in the Galaxy, Large Magellanic Cloud, and Small Magellanic Cloud
We have derived far-ultraviolet extinction curves for stars in theGalaxy, LMC, and SMC from spectra of pairs of stars observed with theFar Ultraviolet Spectroscopic Explorer (FUSE) satellite, matched inspectral type and with different amounts of reddening. The stars wereobserved for other FUSE programs and were not selected for largereddening. Thus, uncertainties in the derived extinction curves dependon the photometric data. In the case of strongly reddened stars from theGalaxy, the strong H2 absorption at the shortest wavelengthsis an additional complication. These initial results indicate that thereis a family of extinction curves that rise strongly to the Lyman limitand extend the related extinction curves from longer wavelengths. Basedon observations made with the NASA-CNES-CSA Far UltravioletSpectroscopic Explorer. FUSE is operated for NASA by Johns HopkinsUniversity under NASA contract NAS5-3298.
| IUE Absorption-Line Observations of the Moderately and Highly Ionized Interstellar Medium toward 164 Early-Type Stars
We present measurements of Galactic interstellar Al III, Si IV, and C IVabsorption recorded in high-resolution archival ultraviolet spectra of164 hot early-type stars observed by the International UltravioletExplorer (IUE) satellite. The objects studied were drawn from the listof hot stars scheduled to be observed with the Far UltravioletSpectroscopic Explorer (FUSE) satellite as part of observing programsdesigned to investigate absorption by O VI in the Galactic disk andhalo. Multiple IUE echelle-mode integrations have been combined toproduce a single ultraviolet (1150-1900 Å) spectrum of each starwith a spectral resolution of ~25 km s-1 (FWHM). Selectedabsorption-line profiles are presented for each star along with plots ofthe apparent column density per unit velocity for each line of the AlIII, Si IV, and C IV doublets. We report absorption-line equivalentwidths, absorption velocities, and integrated column densities based onthe apparent optical depth method of examining interstellar absorptionlines. We also determine column densities and Doppler parameters fromsingle-component curve-of-growth analyses. The scientific analysis ofthese observations will be undertaken after the FUSE satellite producessimilar measurements for absorption by interstellar O IV, Fe III, S III,and other ions. Based on archival data from observations obtained withthe International Ultraviolet Explorer (IUE) satellite sponsored byNASA, SERC, and ESA.
| Magellanic Cloud-Type Interstellar Dust along Low-Density Sight Lines in the Galaxy
We have studied the UV extinction properties along 30 Galactic sightlines using data from the International Ultraviolet Explorer archivethat have never been previously examined. These distant (d>1 kpc)sight lines were selected to investigate the distribution and physicalconditions of gas located in low-density regions of the Galactic diskand halo. The average densities along these sight lines are extremelylow. It is likely that they are dominated by the warm intercloud mediumand have little contribution from the cold cloud medium. We find that asubsample of these sight lines has extinction curves with weak bumps andvery steep far-UV extinction reminiscent of the Magellanic Clouds. Thesesight lines all lie in the region bounded by325deg<=l<=0deg and-5deg>=b>=-11deg. The gas along these sightlines shows forbidden velocities, which may indicate that the dust hasbeen subject to shocks. This type of low-density sight line may mimicthe environments found in the Magellanic Clouds. Large values of N(CaII)/N(Na I) indicating low depletion are associated with steep far-UVextinction. A possible correlation exists between decreasing bumpstrength and increasing far-UV steepness for extinction curves in theGalaxy and the Magellanic Clouds.
| B Stars as a Diagnostic of Star Formation at Low and High Redshift
We have extended the evolutionary synthesis models by Leitherer et al.by including a new library of B stars generated from the IUEhigh-dispersion spectra archive. We present the library and show how thestellar spectral properties vary according to luminosity classes andspectral types. We have generated synthetic UV spectra for prototypicalyoung stellar populations varying the IMF and the star formation law.Clear signs of age effects are seen in all models. The contribution of Bstars in the UV line spectrum is clearly detected, in particular forgreater ages when O stars have evolved. With the addition of the newlibrary we are able to investigate the fraction of stellar andinterstellar contributions and the variation in the spectral shapes ofintense lines. We have used our models to date the spectrum of the localsuper-star cluster NGC 1705-1. Photospheric lines of C III λ1247,Si III λ1417, and S V λ1502 were used as diagnostics todate the burst of NGC 1705-1 at 10 Myr. Interstellar lines are clearlyseen in the NGC 1705-1 spectrum. Broadening and blueshifts of severalresonance lines are stronger in the galaxy spectrum than in our modelsand are confirmed to be intrinsic of the galaxy. Si II λ1261 andAl II λ1671 were found to be pure interstellar lines with anaverage blueshift of 78 km s-1 owing to a directed outflow ofthe interstellar medium. We have selected the star-forming galaxy1512-cB58 as a first application of the new models to high-z galaxies.This galaxy is at z=2.723, it is gravitationally lensed, and its highsignal-to-noise ratio Keck spectrum shows features typical of localstarburst galaxies, such as NGC 1705-1. Models with continuous starformation were found to be more adequate for 1512-cB58 since there arespectral features typical of a composite stellar population of O and Bstars. A model with Z=0.4 Zsolar and an IMF with α=2.8reproduces the stellar features of the 1512-cB58 spectrum.
| GHRS and ORFEUS II Observations of the Highly Ionized Interstellar Medium toward ESO 141-055
We present Goddard High Resolution Spectrograph (GHRS) and ORFEUS IImeasurements of Si IV, C IV, N V, and O VI absorption in theinterstellar medium of the Galactic disk and halo toward the nucleus ofthe Seyfert galaxy ESO 141-055. The high-ionization absorption isstrong, with line strengths consistent with the spectral signatureexpected for hot (T>~10^5 K) collisionally ionized gas in either a``Galactic fountain'' or an inhomogeneous medium containing a mixture ofconductive interfaces and turbulent mixing layers. The total O VI columndensity of ~10^15 cm^-2 suggests that the scale height of O VI is large(>~3 kpc) in this direction. Models of the C IV velocity distributionalong the sight line are consistent with a large scale height for thehighly ionized gas. Comparison of the high ion column densities withmeasurements for other sight lines indicates that the highly ionized gasdistribution is patchy. The amount of O VI perpendicular to the Galacticplane varies by at least a factor of ~4 among the complete halo sightlines thus far studied. In addition to the high ion absorption, lines oflow-ionization species are also present in the spectra. With thepossible exception of Ar I, which may have a lower than expectedabundance resulting from partial photoionization of gas along the sightline, the absorption strengths are typical of those expected for thewarm, neutral interstellar medium. The sight line intercepts a coldmolecular cloud with N(H_2)~10^19 cm^-2. The cloud has an identifiablecounterpart in IRAS 100 μm emission maps of this region of the sky.We detect a Lyα absorber associated with ESO 141-055 at z=0.03492.This study presents an enticing glimpse into the interstellar andintergalactic absorption patterns that will be observed at high spectralresolution by the Far Ultraviolet Spectroscopic Explorer.
| The structure of the interstellar gas towards stars in the globular cluster NGC 6541
Observations are presented of high resolution interstellar Na I D and KI (lambda 7699 Angstroms) line profiles towards 7 stars in the globularcluster NGC 6541 and 3 field stars within 3°\ ofthe cluster. It is seen that the gas in this general direction (l, b ~350°, -11°) shows a complex structure, having the greatestnumber of components yet identified in one of our cluster sightlines,with absorption components detected over an LSR velocity range ~ -100 to+100 km s(-1) . We consider, as far as possible, the identification ofthe observed gas components. In the low-velocity gas we identify theextensive and nearby diffuse gas which contains the cold, dark andmolecular clouds observed closer to the Galactic plane. Components aretentatively identified with both positive and negative peculiar velocitygas components produced by outlying gas in the Sagittarius arm, with gasin the Scutum-Crux and the 3 kpc arms, with an H I filament detected inradio mapping and with shell-like structures expanding from the Sco-Cenassociation. From the cluster star spectra some variability in the finescale gas structure is seen on a scale of a few arcsecs.
| LS 4825: A Blue Supergiant on the Far Side of the Galaxy
We present high-resolution spectroscopic observations of LS 4825, a V =12 B-type star in the Galactic center direction. On the basis of itsstellar and interstellar spectra, we infer that it is likely to be ayoung supergiant at a distance of 21 +/- 5 kpc, and hence lying on thefar side of the Galaxy. Adopting this hypothesis, a differentialabundance analysis shows LS 4825 to have a chemical composition that isconsistent with local B-type supergiants. These observations thereforerepresent the first detailed investigation of a star on the far side ofthe Galactic center. We trace multiple interstellar components in Ca IIK and Na I D spectra, with velocities -206 <= vlsr <= +93 km s-1.We consider the likely origin of this gas and find that some componentsappear to trace matter lying close to the Galactic center. We discussthe possible use of such sight lines in furthering our understandingboth of the nature of gas around the Galactic center and of theabundance gradient of the Galaxy.
| Metallicities of 4 blue supergiants near the Galactic centre.
High resolution optical spectra of four blue supergiants (HD 148422B0.5Ib; HD 178487 B0.5Ib; HD 179407 B1Ib, HD 163522 B1Ib) which liewithin 4.5kpc of the Galactic centre are presented. Careful differentialLTE model atmosphere analyses are used to quantify the differences inphotospheric metal abundances between these stars and MK spectralstandards in the solar neighborhood. A detailed non-LTE model atmosphereanalysis of one star (HD 163522) confirms that the LTE differentialabundances should be reliable, provided we use a comparison star withsimilar atmospheric parameters. One star (HD 148422; R_g_=4.5kpc) has achemical composition similar to normal nearby B-type stars while HD178487 (R_g_=4.1kpc) shows a mild but consistent pattern of a metalenhanced atmosphere (with elements up by 0.1-0.3dex). The other twostars HD 163522 (R_g_=4.1kpc) and HD 179407 (R_g_=3.5kpc) havesignificantly higher metal compositions than their standard comparisonstars with abundances enhanced by 0.30-0.40dex and 0.20-0.5dexrespectively. All of the stars lie outside the Galactic plane (withdistances in the range 0.5
| Absorption by Highly Ionized Interstellar Gas Along Extragalactic and Galactic Sight Lines
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1997AJ....113.2158S&db_key=AST
| High-Resolution Ultraviolet Observations of the Highly Ionized Interstellar Gas toward Radio Loops I and IV
We present new Goddard High-Resolution Spectrograph (GHRS) echelleobservations of the high ionization lines of Si IV, C IV, and N V towardHD 119608, a halo star at d = 4.1 kpc behind the Loop I and IV supernovaremnants. Absorption along the path to HD 119608 makes it possible tostudy energetic processes that may result in the flow of gas into theGalactic halo. The data have a resolution (FWHM) of ~3.5 km s-1 and S/Nratios of 30:1--50:1. The integrated high ion column densities log N =13.57 +/- 0.02, 14.48 +/- 0.06, and 13.45 +/- 0.07 for Si IV, C IV, andN V, respectively, imply a factor of 2--4 enhancement in the amount ofhighly ionized gas compared to average sight lines through the Galacticdisk and halo. The integrated high ion column density ratios, N(CIV)/N(Si IV) = 8.1 +/- 1.1 and N(C IV)/N(N V) = 10.7 +/- 2.1, are alsoseveral times larger than normal. These high ion results suggest theabsorption is influenced by passage of the sight line through the centerof Loop IV. The HD 119608 C IV absorption profile has a bimodal velocitystructure indicative of an expanding shell; we tentatively derive anexpansion velocity of 16 km s-1 for Radio Loop IV. A detailed analysisof the high ion profile structure indicates that multiple types ofhighly ionized gas with a range of properties exist along this sightline. We also reexamine the high ionization properties of the QSO 3C 273sight line using new intermediate-resolution (FWHM ~ 20 km s-1) GHRSdata. We obtain log N = 14.49 +/- 0.03 and 13.87 +/- 0.06 for C IV and NV, respectively. The C IV column density, which is 0.12 dex smaller thanearlier estimates, leads to somewhat smaller ionic ratios thanpreviously determined. We find N(C IV)/N(Si IV) = 5.1 +/- 0.6 and N(CIV)/N(N V) = 4.2 +/- 0.6. However, as for HD 119608, the high ion columndensities toward 3C 273 are larger than normal by factors of 2--4. The3C 273 high ion absorption profiles are much broader than those seentoward HD 119608 and other sight lines near the center of Loop IV. Thelarger line widths may result because the sight line passes through theturbulent edge of Loop IV as well as the X-ray and radio continuumemission regions of the North Polar Spur. We have compiled a list of thehighest quality IUE and GHRS high ion measurements available forinterstellar sight lines through the disk and halo and find thefollowing median averaged results: N(C IV)/N(Si IV) = 3.8 +/- 1.9 andN(C IV)/N(N V) = 4.0 +/- 2.4. These ratios are lower than those foundfor four Loop IV sight lines. We suggest a model for the production ofhighly ionized gas in Loop IV in which the contributions from turbulentmixing layers and conductive interfaces/SNR bubbles to the total highion column densities are approximately equal. Much of the high ionabsorption toward HD 119608 and 3C 273 may occur within a highlyfragmented medium within the remnant or the outer cavity walls of theremnant.
| Cross-correlation characteristics of OB stars from IUE spectroscopy
We present a catalogue of homogeneous measures of the linewidthparameter, v_esin i, for 373 O-type stars and early B supergiants(including the separate components of 25 binary and three triplesystems), produced by cross-correlating high-resolution,short-wavelength IUE spectra against a `template' spectrum of tauSco. Wealso tabulate terminal velocities. There are no O supergiants in oursample with v_esin i<65 km s^-1, and only one supergiant earlier thanB5 has v_esin i<50 km s^-1, confirming that an important linebroadening mechanism in addition to rotation must be present in theseobjects. A calibration of the area under the cross-correlation peakagainst spectral type is used to obtain estimates of continuum intensityratios of the components in 28 spectroscopically binary or multiplesystems. At least seven SB2 systems show evidence for the `Struve-Sahadeeffect', a systematic variation in relative line strength as a functionof orbital phase. The stellar wind profiles of the most rapid rotator inour sample, the O9III:n* star HD 191423 (v_esin i=436km s^-1), show itto have a `wind-compressed disc' similar to that of HD 93521; this starand other rapid rotators are good candidates for studies of non-radialpulsation.
| Further optical and UV spectroscopy of stars in the direction of the Riegel & Crutcher cold cloud
Further optical and UV spectral data are presented for four stars in thedirection of the Riegel & Crutcher cold cloud. Two of the stars lieclose in position to the area covered by our previous optical, UV andradio studies near l=10 deg, while the other two stars lie near l=15deg. The stars range in distance from about 140 pc to 1.5 kpc. The RCcold cloud gas is detected (at a velocity of ~+3 km s^-1) towards a starat a distance of about 150 pc, in agreement with previous cloud distanceestimates. The spectra of the more distant stars contain components athigher velocities; components at +20 and +40 km s^-1 may be identifiedwith peculiar-velocity gas associated with the Sagittarius arm, seenelsewhere in the general field, while a component at -60 km s^-1 may bestellar or interstellar in nature. A component at -20 km s^-1 seentowards previously studied stars in the field is not clearly identifiedin the spectra of the present stars. The atomic column densities of theRiegel & Crutcher cloud component do not vary greatly across thefield, although the CH and CH^+ column densities are more variable. TheCH/CH^+ column density ratio remains fairly constant, however, at avalue that is consistent with the CH^+ being formed in a warm boundarylayer. Along the HD 167264 sightline, the cold gas has an electrondensity of the order of 0.05-0.1 cm^-3 and a space density of the orderof 100-300 cm^-3.
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| An Extension of the Case-Hamburg OB Star Surveys
We have extended the Case-Hamburg OB star surveys to b = +- 30 degreesfor l = +- 60 degres using the Curtis Schmidt telescope and 4 degreeobjective prism at the Cerro Tololo Inter-American Observatory. Acatalog of 234 OB stars and other objects with peculiar spectra ispresented along with finding charts for those objects too faint to beincluded on the BD or CD charts. (SECTION: Stars)
| Interstellar titanium in the galactic halo
We present observations of Ti II lambda 3384 absorption toward 15distant stars in the Galactic halo and the Magellanic Clouds. These newdata extend existing surveys of the distribution of Ti(+) to largerdistances from the plane of the Galaxy than sampled previously, allowingthe scale height of titaniumn to be determined for the first time. Wefind hTi(+ = 1.5 +/- 0.2 kpc, a value which although greaterthan those of other tracers of neutral gas, is not as large as had beensuspected. We interpret the extended distribution of Ti(+) as anindication that its severe depletion in interstellar clouds in the diskis reduced at the lower densities prevailing in the halo. The data areconsistent with a simple power-law dependence of the Ti abundance on theambient density, with exponent k approximately = -1. If the model iscorrect, it implies that refractory elements like Ti are fully returnedto the gas phase at distances beyond approximately 1 kpc from the planeof the Galaxy.
| Probing the galactic disk and halo. 2: Hot interstellar gas toward the inner galaxy star HD 156359
We present Goddard High Resolution Spectrograph intermediate-resolutionmeasurements of the 1233-1256 A spectral region of HD 156396, a halostar at l = 328.7 deg, b = -14.5 deg in the inner Galaxy with a line-ofsight distance of 11.1 kpc and a z-distance of -2.8 kpc. The data have aresolution of 18 km/s Full Width at Half Maximum (FWHM) and asignal-to-noise ratio of approximately 50:1. We detect interstellarlines of Mg II, S II, S II, Ge II, and N V and determine log N/(Mg II) =15.78 +0.25, -0.27, log N(Si II) greater than 13.70, log N(S II) greaterthan 15.76, log N(Ge II) = 12.20 +0.09,-0.11, and log N(N v) = 14.06 +/-0.02. Assuming solar reference abundances, the diffuse clouds containingMg, S, and Ge along the sight line have average logarithmic depletionsD(Mg) = -0.6 +/- 0.3 dex, D(S) greater than -0.2 dex, and D(Ge) = -0.2+/- 0.2 dex. The Mg and Ge depletions are approximately 2 times smallerthan is typical of diffuse clouds in the solar vicinity. Galacticrotational modeling of the N v profiles indicates that the highlyionized gas traced by this ion has a scale height of approximately 1 kpcif gas at large z-distances corotates with the underlying disk gas.Rotational modeling of the Si iv and C iv profiles measured by the IUEsatellite yields similar scale height estimates. The scale heightresults contrast with previous studies of highly ionized gas in theouter Milky Way that reveal a more extended gas distribtion with happroximately equals 3-4 kpc. We detect a high-velocity feature in N vand Si II vLSR approximately equals + 125 km/s) that isprobably created in an interface between warm and hot gas.
| Properties of the highly ionized disk and halo gas toward two distant high-latitude stars
Goddard High Resolution Spectrograph (GHRS) intermediate -resolutionobservations of S III, Si III, Al III, Si IV, C IV, and N V absorptionalong the sight lines to HD 18100 (l = 217.9 deg, b = -62.7, d = 3.1kpc, z = -2.8 kpc) and HD 100340 (l = 258.9 deg, b = +61.2 deg, d = 5.3kpc, z = 4.6 kpc) are presented. These small science aperture spectrahave resolutions ranging from 11 to 20 km/s full width at half maximum(FWHM) and S/N from 30 to 65 per diode substep. Strong absorption bymoderately and highly ionized gas is seen in each direction. Theabsorption in the direction of the south Galactic polar region (HD18100) is kinematically simple, while the absorption in the direction ofnorth Galactic polar region (HD 100304) is kinematically complex. Ineach case the absorption by the highly ionized gas lies within thevelocity range of absorption by neutral and weakly ionized gas. Alongeach sight line, the velocity dispersion determined from the unsaturatedabsorption lines increases with the energy required to create each ion.The logarithmic column densities for Al III, Si IV, C IV, and N V arelog N(atoms/sq cm = 12.71, 13.10, 13.58, and 12.75 toward HD 18100 andlog N = 12.88, 13.31, 13.83, and 13.04 toward HD 100340. Average ionicratios among these species are very similar along the two sight lines.Differences in profile shape between the absorption for AL II, Si IV, CIV, and N V provide additional support for the claim of Savage, Sembach,& Cardelli (1994) that there exists two types of highly ionized gasin the interstellar medium. One type of highly ionized gas isresponsible for the structured Si IV absorption and part of the C IVabsorption. In this gas N(C IV)/N(Si IV) approximately 3.0 and N(CIV)/N(N V) greater than 6. The absorption by this gas seems to beassociated with some type of self-regulating interface or mixing layerbetween the warm and hot interstellar medium. The other type of highlyionized gas is responsible for most of the N V absorption, part of the CIV absorption, and has very little associated Si IV absorption. In thisgas N(C IV)/N(N V) is approximately 1 to 3. This gas is hot (T greaterthan 2 x 105 K) and may be tracing the cooling gas ofsupernova (SN) bubbles or a Galactic fountain. The relative mixture ofthese two types of highly ionized gas varies from one sight line to thenext. The two sight lines in this study sample halo gas in the solarneighborhood and have a smaller percentage of the more highly ionizedgas than inner Galaxy sight lines.
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| Takýmyýldýz: | Akrep |
| Sað Açýklýk: | 17h58m35.23s |
| Yükselim: | -42°29'10.1" |
| Görünürdeki Parlaklýk: | 8.422 |
| Uzaklýk: | 10000000 parsek |
| özdevim Sað Açýklýk: | 3.2 |
| özdevim Yükselim: | -1.1 |
| B-T magnitude: | 8.39 |
| V-T magnitude: | 8.42 |
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