- ID:
- ivo://CDS.VizieR/J/A+A/557/A138
- Title:
- Detailed chemical abundances in the GlC NGC 362
- Short Name:
- J/A+A/557/A138
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We obtained FLAMES GIRAFFE+UVES spectra for both first and second-generation red giant branch (RGB) stars in the globular cluster (GC) NGC 362 and used them to derive abundances of 21 atomic species for a sample of 92 stars. The surveyed elements include proton-capture (O, Na, Mg, Al, Si), alpha-capture (Ca, Ti), Fe-peak (Sc, V, Mn, Co, Ni, Cu), and neutron-capture elements (Y, Zr, Ba, La, Ce, Nd, Eu, Dy). The analysis is fully consistent with that presented for twenty GCs in previous papers of this series. Stars in NGC 362 seem to be clustered into two discrete groups along the Na-O anti-correlation, with a gap at [O/Na]~0dex. Na-rich, second generation stars show a trend to be more centrally concentrated, although the level of confidence is not very high. When compared to the classical second-parameter twin NGC 288, with similar metallicity, but different horizontal branch type and much lower total mass, the proton-capture processing in stars of NGC 362 seems to be more extreme, confirming previous analysis. We discovered the presence of a secondary RGB sequence, redder than the bulk of the RGB: a preliminary estimate shows that this sequence comprises about 6% of RGB stars. Our spectroscopic data and literature photometry indicate that this sequence is populated almost exclusively by giants rich in Ba, and probably rich in all s-process elements, as found in other clusters. In this regards, NGC 362 joins previously studied GCs like NGC 1851, NGC 6656 (M 22), and NGC 7089 (M 2).
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Search Results
- ID:
- ivo://CDS.VizieR/J/ApJS/186/427
- Title:
- Detailed morphology of SDSS galaxies
- Short Name:
- J/ApJS/186/427
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. <II/267>). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01<z<0.1 down to an apparent extinction-corrected limit of g<16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.
- ID:
- ivo://CDS.VizieR/J/MNRAS/478/1763
- Title:
- Detectability of radio emission from exoplanets
- Short Name:
- J/MNRAS/478/1763
- Date:
- 19 Jan 2022 00:23:37
- Publisher:
- CDS
- Description:
- Like the magnetized planets in our Solar system, magnetized exoplanets should emit strongly at radio wavelengths. Radio emission directly traces the planetary magnetic fields and radio detections can place constraints on the physical parameters of these features. Large comparative studies of predicted radio emission characteristics for the known population of exoplanets help to identify what physical parameters could be the key for producing bright, observable radio emission. Since the last comparative study, many thousands of exoplanets have been discovered. We report new estimates for the radio flux densities and maximum emission frequencies for the current population of known exoplanets orbiting pre-main-sequence and main-sequence stars with spectral types F-M. The set of exoplanets predicted to produce observable radio emission are Hot Jupiters orbiting young stars. The youth of these systems predicts strong stellar magnetic fields and/or dense winds, which are the key for producing bright, observable radio emission. We use a new all-sky circular polarization Murchison Widefield Array survey to place sensitive limits on 200MHz emission from exoplanets, with 3{sigma} values ranging from 4.0 to 45.0mJy. Using a targeted Giant Metrewave Radio Telescope observing campaign, we also report a 3{sigma} upper limit of 4.5mJy on the radio emission from V830 Tau b, the first Hot Jupiter to be discovered orbiting a pre-main-sequence star. Our limit is the first to be reported for the low-frequency radio emission from this source.
4794. Detected CH_2_ spectra
- ID:
- ivo://CDS.VizieR/J/A+A/647/A42
- Title:
- Detected CH_2_ spectra
- Short Name:
- J/A+A/647/A42
- Date:
- 19 Jan 2022 13:29:47
- Publisher:
- CDS
- Description:
- The N_KaKc_=4_04_-3_13_ transitions of ortho-CH_2_ between 68 and 71GHz were first detected toward the Orion-KL and W51 Main star-forming regions. Given their high upper level energies (225K) above the ground state, they were naturally thought to arise in dense, hot molecular cores near newly formed stars. However, this has not been confirmed by further observations of these lines and their origin has remained unclear. Quite in general, only a paucity of observational data exist for CH_2_ and, while astrochemically an important compound, its actual occurrence in astronomical sources is poorly constrained. In this work, we aim to investigate the nature of the elusive CH_2_ emission and address its association with hot cores and examine alternative possibilities for its origin. Owing to its importance in carbon chemistry, we also extend the search for CH_2_ lines by observing an assortment of regions guided by the hypothesis that the observed CH_2_ emission likely arises from the hot gas environment of photodissociation regions (PDRs). We carried out observations using, first, the Kitt Peak 12m telescope to verify the original detection of CH_2_ toward different positions in the central region of Orion Molecular Cloud 1. These were followed-up by deep integrations using the higher angular resolution of the Onsala 20 m telescope. We have also searched for the N_KaKc_=2_12_-3_03_ transitions of para-CH_2_ between 440-445GHz toward the Orion giant molecular cloud complex using the APEX 12m telescope. We also obtained auxiliary data for carbon recombination lines with the Effelsberg 100m telescope and employed archival far infrared data. Our and other recent observations of the Orion region reported here, rule out an association with hot and dense gas. We find that the distribution of the CH_2_ emission follows closely that of the [CII] 158 um emission while CH_2_ is undetected toward the hot core itself. The observations suggest that its extended emission rather arises from hot but dilute layers of PDRs, but not from the denser parts of such regions, in particular the Orion Bar. This hypothesis was corroborated by comparisons of the observed CH_2_ line profiles with those of carbon radio recombination lines (CRRLs), well known PDR tracers. In addition, we report the detection of the 70GHz fine-, and hyperfine structure components of ortho-CH_2_ toward the W51 E, W51 M, W51 N, W49 N, W43, W75 N, DR21, and S140 star-forming regions, and three of the N_KaKc_=4_04_-3_13_ fine- and hyperfine structure transitions between 68-71GHz toward W3 IRS5. While we have no information on CH_2_'s spatial distribution in these regions, except for W51, we again see a correspondence of the profiles of CH_2_ lines with those of CRRLs. We see stronger CH_2_ emission toward the extended HII region W51 M than toward the much more massive and denser W51 E and N regions, strongly supporting an origin of CH_2_ in extended dilute gas. We also report the non-detection of the 2_12_-3_03_ transitions of para-CH_2_ toward Orion. Furthermore, using a non-LTE radiative transfer analysis, we can constrain the gas temperatures and H_2_ density to (163+/-26)K and (3.4+/-0.3)x10^3^cm^-3^, respectively, for the 68-71GHz ortho-CH_2_ transitions toward W3 IRS5, for which we have the highest quality data set. This analysis confirms our hypothesis that CH_2_ originates in warm and dilute PDR layers. Our analysis suggests that for the excitation conditions under the physical conditions that prevail in such an environment, these lines are masering, with weak level inversion. The resulting amplification of the lines' spontaneous emission greatly aides their detection.
- ID:
- ivo://CDS.VizieR/J/other/Sci/330.653
- Title:
- Detected planets in the Eta-Earth Survey
- Short Name:
- J/other/Sci/330.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The questions of how planets form and how common Earth-like planets are can be addressed by measuring the distribution of exoplanet masses and orbital periods. We report the occurrence rate of close-in planets (with orbital periods less than 50 days), based on precise Doppler measurements of 166 Sun-like stars. We measured increasing planet occurrence with decreasing planet mass (M). Extrapolation of a power-law mass distribution fitted to our measurements, df/dlogM=0.39M^-0.48^, predicts that 23% of stars harbor a close-in Earth-mass planet (ranging from 0.5 to 2.0 Earth masses). Theoretical models of planet formation predict a deficit of planets in the domain from 5 to 30 Earth masses and with orbital periods less than 50 days. This region of parameter space is in fact well populated, implying that such models need substantial revision.
- ID:
- ivo://CDS.VizieR/J/A+A/372/85
- Title:
- Detected sources at 12{mu}m in 47 Tuc
- Short Name:
- J/A+A/372/85
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The present paper investigates the properties of the dust mass loss in stars populating the giant branch of the globular cluster 47 Tuc, by combining ISOCAM and DENIS data. Raster maps of 5 fields covering areas ranging from 4x4 to 15x15arcmin^2^ at different distances from the center of the cluster have been obtained with ISOCAM at 11.5{mu}m (LW10 filter). The covered fields include most of the red variables known in this cluster. A detection threshold of about 0.2 mJy is achieved, allowing us to detect giant stars at 11.5{mu}m all the way down to the horizontal branch. No dust-enshrouded asymptotic giant branch stars have been found in the observed fields, contrary to the situation encountered in LMC/SMC globular clusters with larger turnoff masses. The color index [12]-[2] (based on the ISO 11.5{mu}m flux and on the DENIS K_S_ magnitude) is used as a diagnostic of dust emission (and hence dust mass loss). Its evolution with luminosity along the giant branch reveals that dust mass loss is only present in V3 (the only cluster Mira variable observed in the present study) and in V18, a star presenting intermittent variability. This conclusion confirms the importance of stellar pulsations in the dust formation and ensuing mass loss.
- ID:
- ivo://CDS.VizieR/J/ApJ/792/43
- Title:
- Detected sources in the region of Magellanic Stream
- Short Name:
- J/ApJ/792/43
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a study of the discrete clouds and filaments in the Magellanic Stream using a new high-resolution survey of neutral hydrogen (H I) conducted with the H75 array of the Australia Telescope Compact Array, complemented by single-dish data from the Parkes Galactic All-Sky Survey. From the individual and combined data sets, we have compiled a catalog of 251 clouds and listed their basic parameters, including a morphological description useful for identifying cloud interactions. We find an unexpectedly large number of head-tail clouds in the region. The implication for the formation mechanism and evolution is discussed. The filaments appear to originate entirely from the Small Magellanic Cloud and extend into the northern end of the Magellanic Bridge.
- ID:
- ivo://CDS.VizieR/J/MNRAS/472/1850
- Title:
- Detecting damped Ly{alpha} absorbers
- Short Name:
- J/MNRAS/472/1850
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We develop an automated technique for detecting damped Ly{alpha} absorbers (DLAs) along spectroscopic lines of sight to quasi-stellar objects (QSOs or quasars). The detection of DLAs in large-scale spectroscopic surveys such as SDSS III sheds light on galaxy formation at high redshift, showing the nucleation of galaxies from diffuse gas. We use nearly 50000 QSO spectra to learn a novel tailored Gaussian process model for quasar emission spectra, which we apply to the DLA detection problem via Bayesian model selection. We propose models for identifying an arbitrary number of DLAs along a given line of sight. We demonstrate our method's effectiveness using a large-scale validation experiment, with excellent performance. We also provide a catalogue of our results applied to 162858 spectra from SDSS-III data release 12.
- ID:
- ivo://CDS.VizieR/J/ApJ/770/L13
- Title:
- Detection of CH_3_COOCH_3_ in Orion
- Short Name:
- J/ApJ/770/L13
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report on the discovery of methyl acetate, CH_3_COOCH_3_, through the detection of a large number of rotational lines from each one of the spin states of the molecule: AA species (A_1_ or A_2_), EA species (E_1_), AE species (E_2_), and EE species (E_3_ or E_4_). We also report, for the first time in space, the detection of the gauche conformer of ethyl formate, CH_3_CH_2_OCOH, in the same source. The trans conformer is also detected for the first time outside the Galactic center source SgrB2. From the derived velocity of the emission of methyl acetate, we conclude that it arises mainly from the compact ridge region with a total column density of (4.2+/-0.5)x10^15^/cm2. The derived rotational temperature is 150K. The column density for each conformer of ethyl formate, trans and gauche, is (4.5+/-1.0)x10^14^/cm2. Their abundance ratio indicates a kinetic temperature of 135K for the emitting gas and suggests that gas-phase reactions could participate efficiently in the formation of both conformers in addition to cold ice mantle reactions on the surface of dust grains.
- ID:
- ivo://CDS.VizieR/J/ApJ/688/L83
- Title:
- Detection of C_5_N^-^ in IRC +10216
- Short Name:
- J/ApJ/688/L83
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report the detection in the envelope of the C-rich star IRC+10216 of four series of lines with harmonically related frequencies: B1389, B1390, B1394, and B1401. The four series must arise from linear molecules with mass and size close to those of C_6_H and C_5_N. Three of the series have half-integer rotational quantum numbers; we assign them to the ^2^{Delta} and ^2^{Sigma}^-^ vibronic states of C_6_H in its lowest ({nu}_11_) bending mode. The fourth series, B1389, has integer J with no evidence of fine or hyperfine structure; it has a rotational constant of 1388.860(2)MHz and a centrifugal distortion constant of 33(1)Hz; it is almost certainly the C_5_N^-^ anion.