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- ID:
- ivo://CDS.VizieR/J/MNRAS/465/2120
- Title:
- Correcting CIV-based virial black hole masses
- Short Name:
- J/MNRAS/465/2120
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The CIV{lambda}{lambda}1498,1501 broad emission line is visible in optical spectra to redshifts exceeding z~5. CIV has long been known to exhibit significant displacements to the blue and these 'blueshifts' almost certainly signal the presence of strong outflows. As a consequence, single-epoch virial black hole (BH) mass estimates derived from CIV velocity widths are known to be systematically biased compared to masses from the hydrogen Balmer lines. Using a large sample of 230 high-luminosity (L_Bol_=10^45.5^-10^48^erg/s), redshift 1.5<z<4.0 quasars with both CIV and Balmer line spectra, we have quantified the bias in CIV BH masses as a function of the CIV blueshift. CIV BH masses are shown to be a factor of 5 larger than the corresponding Balmer-line masses at C IV blueshifts of 3000km/s and are overestimated by almost an order of magnitude at the most extreme blueshifts, ?=5000km/s. Using the monotonically increasing relationship between the CIV blueshift and the mass ratio BH(CIV)/BH(H{alpha}), we derive an empirical correction to all CIV BH masses. The scatter between the corrected CIV masses and the Balmer masses is 0.24dex at low CIV blueshifts (~0km/s) and just 0.10dex at high blueshifts (~3000km/s), compared to 0.40dex before the correction. The correction depends only on the CIV line properties - i.e. full width at half-maximum and blueshift - and can therefore be applied to all quasars where CIV emission line properties have been measured, enabling the derivation of unbiased virial BH-mass estimates for the majority of high-luminosity, high-redshift, spectroscopically confirmed quasars in the literature.
- ID:
- ivo://CDS.VizieR/J/MNRAS/484/L8
- Title:
- Correcting HIRES/Keck RVs for systematic errors
- Short Name:
- J/MNRAS/484/L8
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The HIRES spectrograph, mounted on the 10-m Keck-I telescope, belongs to a small group of radial-velocity (RV) instruments that produce stellar RVs with long-term precision down to ~1m/s. In 2017, the HIRES team published 64480 RVs of 1699 stars, collected between 1996 and 2014. In this bank of RVs, we identify a sample of RV-quiet stars, whose RV scatter is <10m/s, and use them to reveal two small but significant nightly zero-point effects: a discontinuous jump, caused by major modifications of the instrument in August 2004, and a long-term drift. The size of the 2004 jump is 1.5+/-0.1m/s, and the slow zero-point variations have a typical magnitude of <1m/s. In addition, we find a small but significant correlation between stellar RVs and the time relative to local midnight, indicative of an average intranight drift of 0.051+/-0.004m/s/h. We correct the 64480 HIRES RVs for the systematic effects we find, and make the corrected RVs publicly available. Our findings demonstrate the importance of observing RV-quiet stars, even in the era of simultaneously-calibrated RV spectrographs. We hope that the corrected HIRES RVs will facilitate the search for new planet candidates around the observed stars.
- ID:
- ivo://org.gavo.dc/ucac3/q/corr
- Title:
- Corrections between UCAC3 and PPMXL
- Short Name:
- UCAC3 ICRS corr
- Date:
- 15 Aug 2024 15:17:13
- Publisher:
- The GAVO DC team
- Description:
- Differences between UCAC3 and PPMXL in positions and proper motions, on an all-sky one-degree grid. At each gridpoint we give the differences X(PPMXL)- X(UCAC3) averaged over all stars in a sqrt(2)/2-degrees environment around the gridpoint given. The corrections given here should bring UCAC3 based astrometry to the ICRS.
- ID:
- ivo://org.gavo.dc/ppmxl/q/corr
- Title:
- Corrections between USNO-B and PPMXL
- Short Name:
- PPMXL USNO corr
- Date:
- 15 Aug 2024 15:17:01
- Publisher:
- The GAVO DC team
- Description:
- Differences between USNO-B and PPMXL in positions and proper motions, on an all-sky one-degree grid. At each gridpoint we give the differences X(PPMXL)- X(USNO-B1.0) averaged over all stars in a sqrt(2)/2-degrees environment around the gridpoint given. The corrections given here should bring USNO-B based astrometry to the ICRS.
- ID:
- ivo://CDS.VizieR/J/other/Ser/177.109
- Title:
- Corrections to HIP proper motions
- Short Name:
- J/other/Ser/177.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We used the data on latitude variations obtained from observations with 10 classical photographic zenith tubes (PZT) in order to improve the Hipparcos proper motions in declinations µ<SUB>δ</SUB> for 807 stars. Part of observing programmes, carried out during the last century for the purpose of studying the Earth's rotation, were realized by using PZT instruments. These observations were performed within in the intervals (tens of years) much longer than that of the Hipparcos mission (less than 4 years). In addition, the annual number of observations for every PZT- programme star is several hundreds on the average. Though the accuracy of the star coordinates in the Hipparcos Catalogue is by two orders of magnitude better than that of the star coordinates from the PZT observations, the large number of observations performed a much longer time interval makes it possible to correct the Hipparcos proper motions and to improve their accuracy with respect to the accuracy given in the Hipparcos Catalogue. Long term examinations of latitude and time variations were used to form the Earth Orientation Catalogue (EOC-2), aimed at a more accurate determination of positions and proper motions for the stars included. Our method of calculating the corrections of the proper motions in declination from the latitude variations is different from the method used in obtaining the EOC-2 Catalogue. Comparing the results we have established a good agreement between our µ<SUB>δ</SUB> and the EOC-2 ones for the star sample used in the present paper.
- ID:
- ivo://CDS.VizieR/J/other/PASA/30.4
- Title:
- Corrections to the VV13 Catalogue
- Short Name:
- J/other/PASA/30.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Fixes are presented to be applied to the Veron-Cetty and Veron (VCV) Quasar Catalogue, 13th edition (Cat. VII/258). These are comprised of 39 deduplicati ons, 380 astrometric moves of 8+ arcseconds of which 31 are over 10 arcminutes, and 30 indicated delistings.
- ID:
- ivo://CDS.VizieR/J/ApJ/752/72
- Title:
- Correlation metallicity / eclipse depth
- Short Name:
- J/ApJ/752/72
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Previous studies of the interior structure of transiting exoplanets have shown that the heavy-element content of gas giants increases with host star metallicity. Since metal-poor planets are less dense and have larger radii than metal-rich planets of the same mass, one might expect that metal-poor stars host a higher proportion of gas giants with large radii than metal-rich stars. Here I present evidence for a negative correlation at the 2.3{sigma} level between eclipse depth and stellar metallicity in the Kepler gas giant candidates. Based on Kendall's {tau} statistics, the probability that eclipse depth depends on star metallicity is 0.981. The correlation is consistent with planets orbiting low-metallicity stars being, on average, larger in comparison with their host stars than planets orbiting metal-rich stars. Furthermore, since metal-rich stars have smaller radii than metal-poor stars of the same mass and age, a uniform population of planets should show a rise in median eclipse depth with [M/H]. The fact that I find the opposite trend indicates that substantial changes in the gas giant interior structure must accompany increasing [M/H]. I investigate whether the known scarcity of giant planets orbiting low-mass stars could masquerade as an eclipse depth-metallicity correlation, given the degeneracy between metallicity and temperature for cool stars in the Kepler Input Catalog. While the eclipse depth-metallicity correlation is not yet on firm statistical footing and will require spectroscopic [Fe/H] measurements for validation, it is an intriguing window into how the interior structure of planets and even the planet formation mechanism may be changing with Galactic chemical evolution.
- ID:
- ivo://CDS.VizieR/J/A+A/566/A66
- Title:
- Correlation of logR'HK with logIH{alpha}
- Short Name:
- J/A+A/566/A66
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The re-emission in the cores of the CaII H & K and H{alpha} lines are well known proxies of stellar activity. However, these activity indices probe different activity phenomena: the first is more sensitive to plage variation, while the other is more sensitive to filaments. In this paper, we study the long-term correlation between logR'_HK_ and logI_H{alpha}_, two indices based on the CaII H & K and H{alpha} lines, respectively, for a sample of 271 FGK stars using measurements obtained over a ~9-year time span. Because stellar activity is one of the main obstacles to the detection of low-mass and long-period planets, understanding this activity index correlation further can give us some hints about the optimal target to focus on ways to correct for these activity effects. We found a great variety of long-term correlations between logR'_HK_ and logI_H{alpha}_. Around 20% of our sample has a strong positive correlation between the indices while about 3% show strong negative correlation. These fractions are compatible with those found for the case of early-M dwarfs. Stars exhibiting a positive correlation have a tendency to be more active when compared to the median of the sample, while stars showing a negative correlation are more present among higher metallicity stars. There is also a tendency for the positively correlated stars to be more present among the coolest stars, a result which is probably due to the activity level effect on the correlation. Activity level and metallicity therefore seem to be playing a role on the correlation between logR'_HK_ and logI_H{alpha}_. Possible explanations based on the influence of filaments for the diversity in the correlations between these indices are discussed in this paper. As a parallel result, we show a way to estimate the effective temperature of FGK dwarfs that exhibit a low activity level by using the H{alpha} index.
- ID:
- ivo://nasa.heasarc/cosbmaps
- Title:
- COS-B Map Product Catalog
- Short Name:
- COS-B
- Date:
- 27 Sep 2024
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The European Space Agency's satellite COS-B was dedicated to gamma-ray astronomy in the energy range 50 MeV to 5 Gev and carried a single spark chamber telescope with approximately a 20 degree field of view. COS-B operated in a highly eccentric polar orbit with apogee around 90000 km between 17 August 1975 and 25 April 1982. During this operational lifetime, COS-B made 65 observations, 15 of which were devoted to high (>20 deg) galactic latitudes. This database is a collection of maps created from the 65 COS-B observation files. The original observation files can be accessed within BROWSE by changing to the COSBRAW database. For each of the COS-B observation files, the analysis package FADMAP was run and the resulting maps, plus GIF images created from these maps, were collected into this database. Each map is a 120 x 120 pixel FITS format image with 0.5 degree pixels. The user may reconstruct any of these maps within the captive account by running FADMAP from the command line after extracting a file from within the COSBRAW database. The parameters used for selecting data for these product map files are embedded keywords in the FITS maps themselves. These parameters are set in FADMAP, and for the maps in this database are set as 'wide open' as possible. That is, except for selecting on each of 4 energy ranges, all other FADMAP parameters were set using broad criteria. To find more information about how to run FADMAP on the raw event's file, the user can access help files within the COSBRAW database or can use the 'fhelp' facility from the command line to gain information about FADMAP. This is a service provided by NASA HEASARC .