- ID:
- ivo://CDS.VizieR/J/ApJS/181/62
- Title:
- Survey of young solar analogs
- Short Name:
- J/ApJS/181/62
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results from an adaptive optics survey for substellar and stellar companions to Sun-like stars. The survey targeted 266 F5-K5 stars in the 3Myr-3Gyr age range with distances of 10-190pc. Results from the survey include the discovery of two brown dwarf companions (HD 49197B and HD 203030B), 24 new stellar binaries, and a triple system. We infer that the frequency of 0.012-0.072M_{sun}_ brown dwarfs in 28-1590AU orbits around young solar analogs is 3.2^+3.1^_-2.7_% (2{sigma} limits). The result demonstrates that the deficiency of substellar companions at wide orbital separations from Sun-like stars is less pronounced than in the radial velocity "brown dwarf desert." We infer that the mass distribution of companions in 28-1590AU orbits around solar-mass stars follows a continuous dN/dM_2_{prop.to}M^-0.4^_2_ relation over the 0.01-1.0M_{sun}_ secondary mass range. While this functional form is similar to that for isolated objects less than 0.1M_{sun}_, over the entire 0.01-1.0M_{sun}_ range, the mass functions of companions and of isolated objects differ significantly. Based on this conclusion and on similar results from other direct imaging and radial velocity companion surveys in the literature, we argue that the companion mass function follows the same universal form over the entire range between 0 and 1590AU in orbital semimajor axis and ~0.01-20M_{sun}_ in companion mass. In this context, the relative dearth of substellar versus stellar secondaries at all orbital separations arises naturally from the inferred form of the companion mass function.
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Search Results
- ID:
- ivo://CDS.VizieR/J/ApJS/219/27
- Title:
- Surveys of asteroid rotation periods using iPTF
- Short Name:
- J/ApJS/219/27
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Two dedicated asteroid rotation-period surveys have been carried out in the R band with ~20 minute cadence using the intermediate Palomar Transient Factory (iPTF) during 2014 January 6-9 and February 20-23. The total survey area covered 174deg^2^ in the ecliptic plane. Reliable rotation periods for 1438 asteroids are obtained from a larger data set of 6551 mostly main-belt asteroids, each with >=10 detections. Analysis of 1751, PTF-based, reliable rotation periods clearly shows the spin barrier at ~2hr for rubble-pile asteroids. We found a new large super-fast rotator, 2005 UW163, and another five candidates as well. For asteroids of 3<D<15km, our spin-rate distribution shows a number decrease along with frequency after 5 rev/day, which is consistent with the results of the Asteroid Light Curve Database. The discrepancy between our work and that of Pravec et al. (update 2014 April 20) comes mainly from asteroids with {Delta}_m_<0.2mag, which could be the result of different survey strategies. For asteroids with D<3km, we see a significant number drop at f=6rev/day. The relatively short YORP effect timescale for small asteroids could have spun up those elongated objects to reach their spin-rate limit resulting in breakup to create such a number deficiency. We also see that the C-type asteroids show a smaller spin-rate limit than the S-type, which agrees with the general impression that C-type asteroids have a lower bulk density than S-type asteroids.
21193. Suzaku Master Catalog
- ID:
- ivo://nasa.heasarc/suzamaster
- Title:
- Suzaku Master Catalog
- Short Name:
- SUZAMASTER
- Date:
- 09 May 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table records high-level information for each Suzaku observation and provides access to the data archive. Each record is associated with a single observation. An observation contains data from all instruments on board Suzaku. The Suzaku satellate operated from July 2005 till September 2015. This database table was generated at the Suzaku proceesing site with the final data reprocessing (September 2016) after the mission stopped operating. During operation, it was updated on daily basis. This is a service provided by NASA HEASARC .
- ID:
- ivo://CDS.VizieR/J/MNRAS/430/60
- Title:
- Suzaku view of highly ionized outflows in AGN
- Short Name:
- J/MNRAS/430/60
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of a new spectroscopic study of Fe K-band absorption in active galactic nuclei (AGN). Using data obtained from the Suzaku public archive we have performed a statistically driven blind search for FeXXV He{alpha} and/or FeXXVI Ly{alpha} absorption lines in a large sample of 51 Type 1.0-1.9 AGN. Through extensive Monte Carlo simulations we find that statistically significant absorption is detected at E>~6.7keV in 20/51 sources at the P_MC_>=95% level, which corresponds to ~40% of the total sample. In all cases, individual absorption lines are detected independently and simultaneously amongst the two (or three) available X-ray imaging spectrometer detectors, which confirms the robustness of the line detections. The most frequently observed outflow phenomenology consists of two discrete absorption troughs corresponding to FeXXV He{alpha} and FeXXVI Ly{alpha} at a common velocity shift. From xstar fitting the mean column density and ionization parameter for the FeK absorption components are log(N_H_/cm^2^)~23 and log({xi}/erg/cm/s)~4.5, respectively. Measured outflow velocities span a continuous range from <1500km/s up to ~100000km/s, with mean and median values of ~0.1c and ~0.056c, respectively. The results of this work are consistent with those recently obtained using XMM-Newton and independently provides strong evidence for the existence of very highly ionized circumnuclear material in a significant fraction of both radio-quiet and radio-loud AGN in the local universe.
- ID:
- ivo://nasa.heasarc/suzakuwam
- Title:
- Suzaku Wide-Band All-Sky Monitor (WAM) Catalog of Event Lightcurves
- Short Name:
- SUZAKUWAM
- Date:
- 09 May 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table contains information of the events detected by the Wide-band All-sky Monitor (WAM) on Suzaku during its ~10 years of operation. Each event has associated data products. The lightcurves are derived from the on-board operating modes that collected the WAM data from each of the sub-detectors. The lightcurves are rates as a function of time in different energy bands, and they can be used with the general FITS tools within HEAsoft or XRONOS. Version 3 of the lightcurves were generated at HEASARC from the version 2 files, and they are now the final versions hosted at both HEASARC and DARTS. This database table reflects version 3 of the data products. <p> Version 2 of the FITS lightcurves and their plots were generated at Saitama University in Japan and a copy hosted at the DARTS archive, located at ISAS (<a href="http://www.darts.isas.ac.jp/pub/suzaku/wam-2.0/">http://www.darts.isas.ac.jp/pub/suzaku/wam-2.0/</a>). This is a service provided by NASA HEASARC .
21196. Suzaku XIS Configuration Log
- ID:
- ivo://nasa.heasarc/suzaxislog
- Title:
- Suzaku XIS Configuration Log
- Short Name:
- SUZAXISLOG
- Date:
- 09 May 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Suzaku XIS detector units can be configured differently depending on how the user chooses the observation to be carried out. This database table records for each Suzaku observation the different XIS configurations during an observation for all XIS units. The set of parameters that can be configured are: datamode (see also edit mode), window size, on-board window discriminator, on-board grading and event threshold. Each record lists for a given XIS the values set for these parameters in the time interval where they are valid within the observation. Therefore for a given XIS there will be as many records as many different configurations are present within an observation. This database table is generated at the Suzaku processing site. During operation, it is updated on daily basis. This is a service provided by NASA HEASARC .
21197. SV Cam BVR light curves
- ID:
- ivo://CDS.VizieR/J/A+A/376/158
- Title:
- SV Cam BVR light curves
- Short Name:
- J/A+A/376/158
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- New BVR light curves and times of minimum light for the short period RS CVn system SV Cam were analysed to derive the physical parameters of the system and the parameters of the third body orbit. The light curves obtained at the TUEBITAK National Observatory during two nights in 2000 show considerable asymmetry and night-to-night variations. The analysis of the light curves is made using Djurasevic's inverse problem method. The Roche model with spotted areas on the hotter primary component yields a good fit to observations. The extensive series of published photoelectric minima times indicate that the eclipsing pair orbits around the common mass center of the triple system with a period of 41.32yr.
- ID:
- ivo://CDS.VizieR/J/A+A/406/193
- Title:
- SV Cam BVR light curves in Feb. 2001 - March 2002
- Short Name:
- J/A+A/406/193
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the analysis of new BVR light curves for the active star SV Cam. The Roche model with spotted areas on the hotter primary component fits satisfactorily all filter observations yielding two spots in intermediate latitudes and covering about 1.5% each of the stellar surface. Both are ~1000K cooler than surrounding photosphere. The comparison with an earlier season (January/February 2000) suggests that the spots probably evolved in area longitude and latitude but basic and preferred orientation from previous season is confirmed. The comparison stars were SAO 1045 (standard) and SAO 1030 (check).
- ID:
- ivo://CDS.VizieR/J/AN/325/424
- Title:
- SV Cam VB differential photometry
- Short Name:
- J/AN/325/424
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present analysis and spot solutions based on yet unpublished B and V photoelectric observations on the active binary system SV Cam, carried out at Piszkesteto Mountain Station of Konkoly Observatory Budapest. The present spot solutions are based on the observed light curves in September 1993 and July 1994. Comparison of recent and older spot solutions - taken from the literature - suggests long term differences, but these divergences might be caused by some differences of the applied computational methods.
- ID:
- ivo://CDS.VizieR/J/A+A/452/1113
- Title:
- S V effective collision strengths
- Short Name:
- J/A+A/452/1113
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Effective collision strengths are presented in this table for all the transitions among the 26 fine-structure levels arising from the 14 lowest LS states of S V, i.e. those with configurations: (2p^6^)3s^2^, 3s3p, 3p^2^, 3s3d, 3s4s, 3p3d. The effective collision strengths have been calculated using the R-matrix method. Each fine-structure level is assigned an index number ranging from 1 to 26, which are noted in the paper as Table 5. The index values are used here in Table 7 to refer to particular transitions, eg. Index 2-8 denotes the 2p(6)3s3p 3PO(J=0)- 2p(6)3p^2^ 3PE(J=1) transition. The effective collision strengths for each transition are presented for electron temperatures ranging from log10(T)=4.0 to log10(T)=6.0 in steps of 0.1.
