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2371. S7 observations with WiFeS of active galaxies
ID:
ivo://CDS.VizieR/J/ApJS/217/12
Title:
S7 observations with WiFeS of active galaxies
Short Name:
J/ApJS/217/12
Date:
21 Oct 2021
Publisher:
CDS
Description:
Here we describe the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) and present results on 64 galaxies drawn from the first data release. The S7 uses the Wide Field Spectrograph (WiFeS) mounted on the ANU 2.3m telescope located at the Siding Spring Observatory to deliver an integral field of 38x25 arcsec at a spectral resolution of R=7000 in the red (530-710nm), and R=3000 in the blue (340-560nm). From these data cubes we have extracted the narrow-line region spectra from a 4 arcsec aperture centered on the nucleus. We also determine the H{beta} and [OIII]{lambda}5007 fluxes in the narrow lines, the nuclear reddening, the reddening-corrected relative intensities of the observed emission lines, and the H{beta} and [OIII]{lambda}5007 luminosities determined from spectra for which the stellar continuum has been removed. We present a set of images of the galaxies in [OIII]{lambda}5007, [NII]{lambda}6584, and H{alpha}, which serve to delineate the spatial extent of the extended narrow-line region and also to reveal the structure and morphology of the surrounding HII regions. Finally, we provide a preliminary discussion of those Seyfert 1 and Seyfert 2 galaxies that display coronal emission lines in order to explore the origin of these lines.
2372. Sodium detection in WASP-69b atmosphere
ID:
ivo://CDS.VizieR/J/A+A/608/A135
Title:
Sodium detection in WASP-69b atmosphere
Short Name:
J/A+A/608/A135
Date:
21 Oct 2021
Publisher:
CDS
Description:
We analyze the transmission spectrum around the Na I doublet at 589nm of the extrasolar planet WASP-69b, and compare the analysis to that of the well-know hot Jupiter HD 189733b. We also present the analysis of the Rossiter-McLaughlin (RM) effect for WASP-69b. We observed two transits of WASP-69b with the HARPS-North spectrograph (R=115 000) at the TNG telescope. We perform a telluric contamination subtraction based on the comparison between the observed spectra and a telluric water model. Then, the common steps of the differential spectroscopy are followed to extract the transmission spectrum. The method is tested with archival transit data of the extensively studied exoplanet HD 189733b, obtained with the HARPS-South spectrograph at ESO 3.6m telescope, and then applied to WASP-69b data. For HD 189733b, we spectrally resolve the NaI doublet and measure line contrasts of 0.72+/-0.05% (D2) and 0.51+/-0.05% (D1), and FWHMs of 0.64+/-0.04{AA} (D2) and 0.60+/-0.06{AA} (D1), in agreement with previously published results. For WASP-69b only the contrast of the D2 line can be measured (5.8+/-0.3%). This corresponds to a detection at the 5sigma-level of excess absorption of 0.5+/-0.1% in a passband of 1.5{AA}. By measuring the RM effect, we get an angular rotation of 0.24^+0.02^_-0.01_rad/day and a sky-projected angle between the stellar rotation axis and the normal of orbit plane of 0.4^+2.0^_-1.9_{deg} FOR wasP-69b. Similar results to those previously presented in the literature are obtained for the RM analysis of HD 189733b.
2373. Sodium excess objects. I. SDSS-DR7
ID:
ivo://CDS.VizieR/J/ApJS/208/7
Title:
Sodium excess objects. I. SDSS-DR7
Short Name:
J/ApJS/208/7
Date:
21 Oct 2021
Publisher:
CDS
Description:
Several studies have reported the presence of sodium excess objects having neutral atomic absorption lines at 5895{AA} (Na.D) and 8190{AA} that are deeper than expected based on stellar population models that match the stellar continuum. The origin of these lines is therefore hotly debated. van Dokkum & Conroy (2010Natur.468..940V) proposed that low-mass stars (<~0.3M_{sun}_) are more prevalent in massive early-type galaxies, which may lead to a strong Na I 8190 line strength. It is necessary to test this prediction, however, against other prominent optical line indices such as Na.D, Mg b, and Fe 5270, which can be measured with a significantly higher signal-to-noise ratio than Na I 8190. We identified a new sample of roughly 1000 Na.D excess objects (NEOs; ~8% of galaxies in the sample) based on Na.D line strength in the redshift range 0.00<=z<=0.08 from the Sloan Digital Sky Survey (SDSS) DR7 through detailed analysis of galaxy spectra. We explore the properties of these new objects here. The novelty of this work is that the galaxies were carefully identified through direct visual inspection of SDSS images, and we systematically compared the properties of NEOs and those of a control sample of galaxies with normal Na.D line strengths. We note that the majority of galaxies with high velocity dispersions ({sigma}_e_>250km/s) show Na.D excesses.
2374. SOFIA Horsehead nebula region datacube
ID:
ivo://CDS.VizieR/J/A+A/595/A34
Title:
SOFIA Horsehead nebula region datacube
Short Name:
J/A+A/595/A34
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a new multi-pixel high resolution (R>~10^7^) spectrometer for the Stratospheric Observatory for far-infrared astronomy (SOFIA). The receiver uses 2x7-pixel subarrays in orthogonal polarization, each in an hexagonal array around a central pixel. We present the first results for this new instrument after commissioning campaigns in May and December 2015 and after science observations performed in May 2016. The receiver is designed to ultimately cover the full 1.8-2.5THz frequency range but in its first implementation, the observing range was limited to observations of the [CII] line at 1.9THz in 2015 and extended to 1.83-2.07THz in 2016. The instrument sensitivities are state-of-the-art and the first scientific observations performed shortly after the commissioning confirm that the time electronic efficiency for large scale imaging is improved by more than an order of magnitude as compared to single pixel receivers. An example of large scale mapping around the Horsehead Nebula is presented here illustrating this improvement. The array has been added to SOFIA's instrument suite already for ongoing observing cycle 4.
2375. SOFIA Massive (SOMA) Star Formation Survey. I.
ID:
ivo://CDS.VizieR/J/ApJ/843/33
Title:
SOFIA Massive (SOMA) Star Formation Survey. I.
Short Name:
J/ApJ/843/33
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present an overview and first results of the Stratospheric Observatory For Infrared Astronomy Massive (SOMA) Star Formation Survey, which is using the FORCAST instrument to image massive protostars from ~10 to 40{mu}m. These wavelengths trace thermal emission from warm dust, which in Core Accretion models mainly emerges from the inner regions of protostellar outflow cavities. Dust in dense core envelopes also imprints characteristic extinction patterns at these wavelengths, causing intensity peaks to shift along the outflow axis and profiles to become more symmetric at longer wavelengths. We present observational results for the first eight protostars in the survey, i.e., multiwavelength images, including some ancillary ground-based mid- infrared (MIR) observations and archival Spitzer and Herschel data. These images generally show extended MIR/FIR emission along directions consistent with those of known outflows and with shorter wavelength peak flux positions displaced from the protostar along the blueshifted, near-facing sides, thus confirming qualitative predictions of Core Accretion models. We then compile spectral energy distributions and use these to derive protostellar properties by fitting theoretical radiative transfer models. Zhang and Tan models, based on the Turbulent Core Model of McKee and Tan, imply the sources have protostellar masses m*~10-50M_{sun}_ accreting at ~10^-4^-10^-3^M_{sun}_/yr inside cores of initial masses Mc~30-500M_{sun}_ embedded in clumps with mass surface densities {Sigma}_cl_~0.1-3g/cm^2^. Fitting the Robitaille et al. models typically leads to slightly higher protostellar masses, but with disk accretion rates ~100x smaller. We discuss reasons for these differences and overall implications of these first survey results for massive star formation theories.
2376. SOIR
ID:
ivo://bira-iasb/soir/soir_q/epn_core
Title:
SOIR
Short Name:
soir.epn_core
Date:
08 Oct 2024 09:26:16
Publisher:
Planetary Atmospheres Research Unit - Royal Belgian Institute for Space Aeronomy
Description:
Profiles of species in Venus atmosphere terminator. Data retrieved from calibrated spectra obtained with the SPICAV-SOIR instrument on board the Venus Express spacecraft. These spectra can be checked on the ESA PSA repository. See: A.C. Vandaele et al., Contribution from SOIR/VEX to the updated Venus International Reference Atmosphere (VIRA), Adv. Space Res. (2015), http://dx.doi.org/10.1016/j.asr:2015.08.012.
2377. Solar disk spectrum (660-1175A)
ID:
ivo://CDS.VizieR/J/A+AS/126/281
Title:
Solar disk spectrum (660-1175A)
Short Name:
J/A+AS/126/281
Date:
21 Oct 2021
Publisher:
CDS
Description:
The near-limb quiet-Sun spectrum recorded on January 25, 1996 near the solar North pole is presented in tabular form and in graphical form. Table 1 - the line list - lists all lines found in the spectrum providing absolute peak intensities, measured and literature wavelengths, identification, and classification of the transition. Fig. 4 is a display the composite spectrum. The most prominent lines are labelled. In this figure intensities are given in instrumental units and logarithmic scale.
2378. Solar flux model in 30-1300nm wavelength range
ID:
ivo://CDS.VizieR/J/ApJS/181/351
Title:
Solar flux model in 30-1300nm wavelength range
Short Name:
J/ApJS/181/351
Date:
21 Oct 2021
Publisher:
CDS
Description:
Solar photon scattering probabilities (g values) have been calculated for discrete transitions in 12 species, in a format designed primarily to allow analysis of spacecraft observations from MESSENGER and BepiColombo at Mercury. The results support observations using the MESSENGER Ultraviolet and Visible Spectrometer spectrograph experiment operating over the spectral range 1150-6000{AA} and the BepiColombo spectrograph in the range 550-3150{AA}. Significant radial velocity dependence is shown for most of the emission lines, a critical factor for interpretation of the observed spectra. The g values have general application for solar system emission sources dominated by scattering of the solar flux.
2379. SOLAR-ISS Spectrum covering 165-3000nm
ID:
ivo://CDS.VizieR/J/other/SoPh/295.14
Title:
SOLAR-ISS Spectrum covering 165-3000nm
Short Name:
J/other/SoPh/295
Date:
21 Oct 2021
Publisher:
CDS
Description:
The accurate measurement of the solar spectrum at the top of the atmosphere and its variability are fundamental inputs for solar physics (Sun modeling), terrestrial atmospheric photochemistry, and Earth's climate (climate's modeling). These inputs were the prime objective set in 1996 for the SOLAR International Space Station (ISS). The SOLAR package represents a set of three solar instruments measuring the total and spectral absolute irradiance from 16nm to 3088nm. SOLAR was launched with the European Columbus space laboratory in February 2008 aboard the NASA Space Shuttle Atlantis. SOLAR on the ISS tracked the Sun until it was decommissioned in February 2017. The SOLar SPECtrum (SOLSPEC) instrument of the SOLAR payload allowed the measurement of solar spectra in the 165-3000nm wavelength range for almost a decade. Until the end of its mission, SOLAR/SOLSPEC was pushed to its limits to test how it was affected by space environmental effects (external thermal factors) and to better calibrate the space-based spectrometer. To that end, a new solar reference spectrum (SOLAR-ISS - V1.1) representative of the 2008 solar minimum was obtained from the measurements made by the SOLAR/SOLSPEC instrument and its calibrations. The main purpose of this article is to improve the SOLAR-ISS reference spectrum (between 165 and 180nm in the far ultraviolet, between 216.9 and 226.8nm in the middle ultraviolet, and between 2400 and 3000nm in the near-infrared). SOLAR-ISS has a resolution better than 0.1nm between 165 and 1000nm, and 1nm in the 1000-3000nm wavelength range. Finally, a first comparison is made between the new SOLAR-ISS spectrum (V2.0) and the Total and Spectral solar Irradiance Sensor (TSIS-1) spectrum obtained from its first observations from the ISS. Indeed, the launch of TSIS in December 2017 provides a new light on the absolute determination of the solar spectrum and especially in the infrared region of the spectrum.
2380. Solar lines from Ceres spectra
ID:
ivo://CDS.VizieR/J/A+A/544/A125
Title:
Solar lines from Ceres spectra
Short Name:
J/A+A/544/A125
Date:
21 Oct 2021
Publisher:
CDS
Description:
Present knowledge of the solar spectrum is limited because it is very difficult to observe the integrated solar spectrum at high resolution. The reflected solar light from asteroids has been shown to provide a relatively straightforward integrated and unmodified solar spectrum. We exploit this methodology to improve our knowledge of solar photospheric line positions both in terms of line number and precision with respect to the available solar line atlas.

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