- ID:
- ivo://CDS.VizieR/J/ApJ/903/33
- Title:
- 1366 LGRB redshifts estimates with BARSE
- Short Name:
- J/ApJ/903/33
- Date:
- 15 Mar 2022
- Publisher:
- CDS
- Description:
- We present a catalog of probabilistic redshift estimates for 1366 individual Long-duration Gamma-ray Bursts (LGRBs) detected by the Burst And Transient Source Experiment (BATSE). This result is based on a careful selection and modeling of the population distribution of 1366 BATSE LGRBs in the five-dimensional space of redshift and the four intrinsic prompt gamma-ray emission properties: the isotropic 1024ms peak luminosity (L_iso_), the total isotropic emission (E_iso_), the spectral peak energy (E_pz_), as well as the intrinsic duration (T_90z_), while carefully taking into account the effects of sample incompleteness and the LGRB-detection mechanism of BATSE. Two fundamental plausible assumptions underlie our purely probabilistic approach: (1) LGRBs trace, either exactly or closely, the cosmic star formation rate, with a possibility of the excess rates of LGRBs in the nearby universe, and (2) the joint four-dimensional distribution of the aforementioned prompt gamma-ray emission properties is well described by a multivariate log-normal distribution. Our modeling approach enables us to constrain the redshifts of individual BATSE LGRBs to within 0.36 and 0.96 average uncertainty ranges at 50% and 90% confidence levels, respectively. Our redshift predictions are completely at odds with the previous redshift estimates of BATSE LGRBs that were computed via the proposed phenomenological high-energy relations, specifically, the apparently strong correlation of LGRBs' peak luminosity with the spectral peak energy, lightcurve variability, and spectral lag. The observed discrepancies between our predictions and the previous works can be explained by the strong influence of detector threshold and sample incompleteness in shaping these phenomenologically proposed high-energy correlations in the literature. Finally, we also discuss the potential effects of an excess cosmic rate of LGRBs at low redshifts and the possibility of a luminosity evolution of LGRBs on our results.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/632/A115
- Title:
- L1188 HCO+, 12CO and 13CO datacubes
- Short Name:
- J/A+A/632/A115
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In order to search for further observational evidence of cloud-cloud collisions in one of the promising candidates, L1188, we carried out observations of multiple molecular lines toward the intersection region of the two nearly orthogonal filamentary molecular clouds in L1188. Based on these observations, we find two parallel filamentary structures, both of which have at least two velocity components being connected with broad bridging features. We also found a spatially complementary distribution between the two molecular clouds, as well as enhanced ^13^CO emission and ^12^CO self-absorption toward their abutting regions. At the most blueshifted velocities, we unveiled a 1pc-long arc ubiquitously showing ^12^CO line wings. We discovered two 22GHz water masers, which are the first maser detections in L1188. An analysis of line ratios at a linear resolution of 0.2 pc suggests that L1188 is characterised by kinetic temperatures of 13-23K and H_2_ number densities of 10^3^-10^3.6^cm^-3^. On the basis of previous theoretical predictions and simulations, we suggest that these observational features can be naturally explained by the scenario of a cloud-cloud collision in L1188, although an additional contribution of stellar feedback from low-mass young stellar objects cannot be ruled out.
7893. L1642 Herschel maps
- ID:
- ivo://CDS.VizieR/J/A+A/563/A125
- Title:
- L1642 Herschel maps
- Short Name:
- J/A+A/563/A125
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- L1642 is one of the two high galactic latitude (|b|>30{deg}) clouds confirmed to have active star formation. We examine the properties of this cloud, especially the large-scale structure, dust properties, and compact sources at different stages of star formation. We present high-resolution far-infrared and submillimetre observations with the Herschel and AKARI satellites and millimetre observations with the AzTEC/ASTE telescope, which we combined with archive data from near- and mid-infrared (2MASS, WISE) to millimetre wavelength observations (Planck).
- ID:
- ivo://CDS.VizieR/I/87B
- Title:
- LHS Catalogue, 2nd Edition
- Short Name:
- I/87B
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The catalogue gathers stars with large proper motions, the large majority coming out of the Bruce Proper Motion Survey (W.J. Luyten). 804 fields in the Palomar Survey have been hand-blinked or processed by an automated blink-machine; 160 low galactic latitude fields could not be handled. There are therefore many less stars with high proper motion south of -33 degrees (limit of the Palomar Survey) compared to the Northern hemisphere. Stars with proper motions larger than 2arcsec/yr are numbered 1 to 100; stars with proper motions between 1 and 2arcsec/yr are numbered 101 to 1000 ; numbers 1001 through 5000 are assigned to stars with proper motions between 0.5 and 1arcsec/yr. The stars which appear to have motions between 0.480 and 0.499arcsec/yr have been assigned numbers larger than 5000. Numbers larger than 6000 refer to Appendix II of the printed publication, containing stars for which at one time or another a value larger than 0.49arcsec/yr was published; these numbers are not listed in the printed version of the catalogue. All proper motions have been reduced to the Palomar-Bruce system. The catalogue supersedes the "Catalogue of Stars with Motions exceeding 0.5" annually" (LFT) published in 1955 (CDS ref. <I/54>)
- ID:
- ivo://CDS.VizieR/J/PASP/117/676
- Title:
- LHS faint proper-motion stars
- Short Name:
- J/PASP/117/676
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present low-resolution spectroscopic observations of faint proper-motion stars from the LHS Catalogue, concentrating on stars with m_r_>16.5 and {mu}>0.5"/yr. The present paper includes observations and spectral classifications for 294 M dwarfs, M subdwarfs (sdM), and extreme M subdwarfs (esdM). We also identify white dwarfs among the faintest LHS stars. We have cross-referenced this sample against the Two Micron All Sky Survey (2MASS) sources, and list data for the detected objects. We discuss stars of individual interest, as well as the characteristics of the overall sample. As expected, a significant number of the stars in this proper-motion-selected sample are halo subdwarfs, including an esdM dwarf, LHS 3481, that is likely to lie within 20pc of the Sun. None of the subdwarfs show H{alpha} emission.
7896. LH 47 UVBRI photometry
- ID:
- ivo://CDS.VizieR/J/A+AS/123/455
- Title:
- LH 47 UVBRI photometry
- Short Name:
- J/A+AS/123/455
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Table 3 lists the final photometric data of our observations. The UBVRI observations were done with the 1.54m Danish telescope at ESO on October 3rd and 4th, 1992. The CCD was ESO#28, a TEK 1024x1024 with a pixel size of 24mue corresponding to 0.377" per pixel. The total field of view is 6.4'x6.4'. A standard reduction was done with MIDAS and IRAF, the photometry was performed with DAOPHOT within IRAF. The images of Oct 4th have been calibrated using the calibration field around PG 0231+051 (Landolt 1992, Cat. <II/183>). The images of Oct 3rd have then been adopted to the system of Oct 4th. The final Table 3 lists 4613 stars with V and B-V information. In addition U-B is available for 1159 of these stars, V-R for 3519 and V-I for 2854 stars. Table 4 gives those stars from our field of view which are present in the MACS (Magellanic Catalogue of Stars; Tucholke et al. 1996, Cat. <I/221>). The table contains the MACS Id., our x and y position and our UBV photometry, and right ascension and declination from the MACS. These stars may serve to calculate an exact position for every star from Table 3 or to define a coordinate grid for comparison with other observations, such as radio or X-ray data.
- ID:
- ivo://CDS.VizieR/J/A+A/651/A84
- Title:
- Li abundance and mixing in giant stars
- Short Name:
- J/A+A/651/A84
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- We aim to constrain the mixing processes in low-mass stars by investigating the behaviour of the Li surface abundance after the main sequence. We take advantage of the data from the sixth internal data release of Gaia-ESO, idr6, and from the Gaia Early Data Release 3, EDR3. We selected a sample of main-sequence, sub-giant, and giant stars in which the Li abundance is measured by the Gaia-ESO survey. These stars belong to 57 open clusters with ages from 130Myr to about 7Gyr and to Milky Way fields, covering a range in [Fe/H] between -1.0 and +0.5dex, with few stars between -1.0 and -2.5dex. We studied the behaviour of the Li abundances as a function of stellar parameters. We inferred the masses of giant stars in clusters from the main-sequence turn-off masses, and for field stars through comparison with stellar evolution models using a maximum likelihood technique. We compared the observed Li behaviour in field giant stars and in giant stars belonging to individual clusters with the predictions of a set of classical models and of models with mixing induced by rotation and thermohaline instability. The comparison with stellar evolution models confirms that classical models cannot reproduce the observed lithium abundances in the metallicity and mass regimes covered by the data. The models that include the effects of both rotation-induced mixing and thermohaline instability account for the Li abundance trends observed in our sample in all metallicity and mass ranges. The differences between the results of the classical models and of the rotation models largely differ (up to~2 dex), making lithium the best element with which to constrain stellar mixing processes in low-mass stars. We discuss the nature of a sample of Li-rich stars. We demonstrate that the evolution of the surface abundance of Li in giant stars is a powerful tool for constraining theoretical stellar evolution models, allowing us to distinguish the effect of different mixing processes. For stars with well-determined masses, we find a better agreement of observed surface abundances and models with rotation-induced and thermohaline mixing. Rotation effects dominate during the main sequence and the first phases of the post-main-sequence evolution, and the thermohaline induced mixing after the bump in the luminosity function.
- ID:
- ivo://CDS.VizieR/J/A+A/562/A92
- Title:
- Li abundance in solar analogues
- Short Name:
- J/A+A/562/A92
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We want to study the effects of the formation of planets and planetary systems on the atmospheric Li abundance of planet host stars. In this work we present new determinations of lithium abundances for 326 main sequence stars with and without planets in the Teff range 5600-5900K. The 277 stars come from the HARPS sample, the remaining targets were observed with a variety of high-resolution spectrographs.
- ID:
- ivo://CDS.VizieR/J/MNRAS/449/4038
- Title:
- Li abundance of giants in 3 globular clusters
- Short Name:
- J/MNRAS/449/4038
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The presence of multiple populations in globular clusters has been well established thanks to high-resolution spectroscopy. It is widely accepted that distinct populations are a consequence of different stellar generations: intra-cluster pollution episodes are required to produce the peculiar chemistry observed in almost all clusters. Unfortunately, the progenitors responsible have left an ambiguous signature and their nature remains unresolved. To constrain the candidate polluters, we have measured lithium and aluminium abundances in more than 180 giants across three systems: NGC 1904, NGC 2808, and NGC 362. The present investigation along with our previous analysis of M12 and M5 affords us the largest database of simultaneous determinations of Li and Al abundances. Our results indicate that Li production has occurred in each of the three clusters. In NGC 362 we detected an M12-like behaviour, with first and second-generation stars sharing very similar Li abundances favouring a progenitor that is able to produce Li, such as AGB stars. Multiple progenitor types are possible in NGC 1904 and NGC 2808, as they possess both an intermediate population comparable in lithium to the first generation stars and also an extreme population, that is enriched in Al but depleted in Li. A simple dilution model fails in reproducing this complex pattern. Finally, the internal Li variation seems to suggest that the production efficiency of this element is a function of the cluster's mass and metallicity - low-mass or relatively metal-rich clusters are more adept at producing Li.
- ID:
- ivo://CDS.VizieR/J/A+A/409/251
- Title:
- Li abundances and velocities in F and G stars
- Short Name:
- J/A+A/409/251
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Lithium abundances have been determined in 127 F and G Pop I stars based on new measurements of the equivalent width of the {lambda}6707{AA} Li I line from their high resolution CCD spectra. Distances and absolute magnitudes of these stars have been obtained from the Hipparcos Catalogue (<I/239>) and their masses and ages derived, enabling us to investigate the behaviour of lithium as a function of these parameters. Based on their location on the HR diagram superposed on theoretical evolutionary tracks, the sample of the stars has been chosen to ensure that they have more or less completed their Li depletion on the main sequence.