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1. Catalogue of Markarian Galaxies
ID:
ivo://CDS.VizieR/VII/61A
Title:
Catalogue of Markarian Galaxies
Short Name:
VII/61A
Date:
21 Oct 2021
Publisher:
CDS
Description:
Markarian galaxies have a moderate to strong ultraviolet continuum as detected by an objective-prism survey at Byurakan Observatory from 1965 to 1978. The survey was done with a 40-inch Schmidt telescope with a dispersion of 2500 angstroms/millimeter at H-alpha. The catalog contains no galaxies brighter than mag 13.0 or fainter than mag 17.5. The catalog fields are Markarian Identification number; S(eyfert) or Q(uasar) flag; cross identifications to other catalogs; B1950 positions; major and minor axis (arcsec); magnitude and spectral types, including a code for the strength of the UV continuum. This catalogue is superseded by the First Byurakan Survey (see the "See Also" section below) The original documentation was by Robert S. Hill and Lee E. Brotzman in the "adc.doc" file (From the CD-ROM "Selected Astronomical Catalogs" Vol. 1 (1992), directory "nonstell/galaxies/mkn")
2. Faint Markarian galaxies of SBS. III.
ID:
ivo://CDS.VizieR/J/AJ/124/1283
Title:
Faint Markarian galaxies of SBS. III.
Short Name:
J/AJ/124/1283
Date:
21 Oct 2021
Publisher:
CDS
Description:
We continue our program of spectroscopic observations of objects from the Second Byurakan Survey (SBS). This survey contains more than 3600 objects with m_pg_<19.5mag, half of them being galaxies and the other half being starlike objects. The aim of this work is to compile a complete sample of faint (B<17) Markarian galaxies. Here we present spectroscopic data for 185 galaxies, obtained with the 6m telescope of the Special Astrophysical Observatory in Russia and the 2.1m telescope of the Guillermo Haro Astrophysical Observatory in Mexico. In the present subsample, we find three new Seyfert 1 galaxies (SBS 0654+598, 1118+541, and 1320+551); one narrow-line Seyfert 1 (SBS 0748+499), one Seyfert 2 (SBS 0925+585), and three Seyfert2/LINER (SBS 0811+584, 1344+527, and 1428+529) galaxies; 12 LINERs; 13 blue compact dwarf galaxies; 65 starburst nuclei; 85 emission-line galaxies; and two absorption galaxies. Relevant astrophysical parameters (magnitude, redshift, relative intensities of emission lines, etc.) are given for the observed galaxies.
3. F-GAMMA 2.64-43GHz radio data over 2007-2015
ID:
ivo://CDS.VizieR/J/A+A/626/A60
Title:
F-GAMMA 2.64-43GHz radio data over 2007-2015
Short Name:
J/A+A/626/A60
Date:
21 Oct 2021
Publisher:
CDS
Description:
The advent of the Fermi gamma-ray space telescope with its superb sensitivity, energy range, and unprecedented capability to monitor the entire 4{pi} sky within less than 2-3 h, introduced a new standard in time domain gamma-ray astronomy. Among several breakthroughs, Fermi has - for the first time - made it possible to investigate, with high cadence, the variability of the broadband spectral energy distribution (SED), especially for active galactic nuclei (AGN). This is necessary for understanding the emission and variability mechanisms in such systems. To explore this new avenue of extragalactic physics the Fermi-GST AGN Multi-frequency Monitoring Alliance (F-GAMMA) programme undertook the task of conducting nearly monthly, broadband radio monitoring of selected blazars, which is the dominant population of the extragalactic gamma-ray sky, from January 2007 to January 2015. In this work we release all the multi-frequency light curves from 2.64 to 43 GHz and first order derivative data products after all necessary post-measurement corrections and quality checks. Along with the demanding task to provide the radio part of the broadband SED in monthly intervals, the F-GAMMA programme was also driven by a series of well-defined fundamental questions immediately relevant to blazar physics. On the basis of the monthly sampled radio SEDs, the F-GAMMA aimed at quantifying and understanding the possible multiband correlation and multi-frequency radio variability, spectral evolution and the associated emission, absorption and variability mechanisms. The location of the gamma-ray production site and the correspondence of structural evolution to radio variability have been among the fundamental aims of the programme. Finally, the programme sought to explore the characteristics and dynamics of the multi-frequency radio linear and circular polarisation. The F-GAMMA ran two main and tightly coordinated observing programmes. The Effelsberg 100 m telescope programme monitoring 2.64, 4.85, 8.35, 10.45, 14.6, 23.05, 32, and 43 GHz, and the IRAM 30 m telescope programme observing at 86.2, 142.3, and 228.9 GHz. The nominal cadence was one month for a total of roughly 60 blazars and targets of opportunity. In a less regular manner the F-GAMMA programme also ran an occasional monitoring with the APEX 12 m telescope at 345 GHz. We only present the Effelsberg dataset in this paper. The higher frequencies data are released elsewhere. The current release includes 155 sources that have been observed at least once by the F-GAMMA programme. That is, the initial sample, the revised sample after the first Fermi release, targets of opportunity, and sources observed in collaboration with a monitoring programme following up on Planck satellite observations. For all these sources we release all the quality-checked Effelsberg multi-frequency light curves. The suite of post-measurement corrections and flagging and a thorough system diagnostic study and error analysis is discussed as an assessment of the data reliability. We also release data products such as flux density moments and spectral indices. The effective cadence after the quality flagging is around one radio SED every 1.3 months. The coherence of each radio SED is around 40 min. The released dataset includes more than 3x104 measurements for some 155 sources over a broad range of frequencies from 2.64 GHz to 43 GHz obtained between 2007 and 2015. The median fractional error at the lowest frequencies (2.64-10.45 GHz) is below 2%. At the highest frequencies (14.6-43 GHz) with limiting factor of the atmospheric conditions, the errors range from 3% to 9%, respectively.
4. First Byurakan Survey (FBS)
ID:
ivo://CDS.VizieR/VII/172
Title:
First Byurakan Survey (FBS)
Short Name:
VII/172
Date:
21 Oct 2021
Publisher:
CDS
Description:
A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (<16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.
5. HST/COS and FUSE UV spectra of Mrk 509
ID:
ivo://CDS.VizieR/J/A+A/623/A82
Title:
HST/COS and FUSE UV spectra of Mrk 509
Short Name:
J/A+A/623/A82
Date:
21 Oct 2021
Publisher:
CDS
Description:
To elucidate the location, physical conditions, mass outflow rate, and kinetic luminosity of the outflow from the active nucleus of the Seyfert 1 galaxy Mrk 509 we used coordinated ultraviolet and X-ray spectral observations in 2012 to followup our lengthier campaign conducted in 2009. We observed Mrk 509 with the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST) on 2012-09-03 and 2012-10-11 coordinated with X-ray observations using the High Energy Transmission Grating on the Chandra X-ray Observatory. Our far-ultraviolet spectra used grating G140L on COS to cover wavelengths from 920-2000{AA} at a resolving power of 2000, and gratings G130M and G160M to cover 1160-1750{AA} at a resolving power of 15000. We detect variability in the blue-shifted UV absorption lines on timescales spanning 3-12 years. The inferred densities in the absorbing gas are greater than logn[cm^-3^]~3. For ionization parameters ranging over logU=-1.5 to -0.2, we constrain the distances of the absorbers to be closer than 220pc to the active nucleus. The impact on the host galaxy appears to be confined to the nuclear region.
6. Markarian galaxies and Zwicky clusters relations
ID:
ivo://CDS.VizieR/J/A+AS/65/349
Title:
Markarian galaxies and Zwicky clusters relations
Short Name:
J/A+AS/65/349
Date:
21 Oct 2021
Publisher:
CDS
Description:
In the same area covered by Markarian survey and CGCG, there are 1344 Markarian galaxies, of which 597 are positioned inside the contours of Zwicky clusters. Data on these galaxies and respective clusters are presented in different tables, according to whether they are galaxies which are members of clusters, or probable or possible members projection cases are considered separately.
7. Michigan Emission-Line Objects
ID:
ivo://CDS.VizieR/VII/171
Title:
Michigan Emission-Line Objects
Short Name:
VII/171
Date:
21 Oct 2021
Publisher:
CDS
Description:
The objects of this catalogue were detected by using the 61-cm aperture Curtis Schmidt telescope in combination with a thin objective prism (1.8{deg}) at the Cerro Tololo Inter-American Observatory. The low-dispersion spectra (174nm/mm at H{beta}) cover the wavelength range between 5350 and 3400 {AA}, where the emission lines such that those of [OII], [OIII] and Ly{alpha} are visible. The objects could be detected up to 18th magnitude. Note that the list archived here is not the same as the published lists (see the "References" section below): the positions in the "catalog.dat" file are generally more accurate than those in the original publication and the origin for these is not known. In the printed lists of papers , information presented for each object also includes image dimensions from the Palomar Observatory Sky Survey, an estimated continuum apparent magnitude, a redshift estimate when feasible, or (for galaxies) a spectral classification which involves compactness, color, and line-strength parameters.
8. Mrk421 in March 2010
ID:
ivo://CDS.VizieR/J/A+A/578/A22
Title:
Mrk421 in March 2010
Short Name:
J/A+A/578/A22
Date:
21 Oct 2021
Publisher:
CDS
Description:
A flare from the TeV blazar Mrk 421, occurring in March 2010, was observed for 13 consecutive days from radio to very high energy (VHE; E>100GeV) gamma-rays with MAGIC, VERITAS, Whipple, FermiLAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We model the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigate the physical parameters, and evaluate whether the observed broadband SED variability can be associated to variations in the relativistic particle population. Flux variability was remarkable in the X-ray and VHE bands while it was minor or not significant in the other bands. The one-zone SSC model can describe reasonably well the SED of each day for the 13 consecutive days. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission while the other smaller zone, which is spatially separated from the first one, contributes to the daily-variable emission occurring in X-rays and VHE gamma-rays. Both the one-zone SSC and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly to the underlying particle population. This shows that the particle acceleration and cooling mechanism producing the radiating particles could be the main one responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement to the observed SED at the narrow peaks of the low- and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by the variation of the parameters related to the emitting region itself ({delta}, B and R), in addition to the parameters related to the particle population.
9. Mrk 421 multi-wavelength variability, 2007-2009
ID:
ivo://CDS.VizieR/J/A+A/593/A91
Title:
Mrk 421 multi-wavelength variability, 2007-2009
Short Name:
J/A+A/593/A91
Date:
21 Oct 2021
Publisher:
CDS
Description:
We perform an extensive multi-band variability and correlation study of the TeV blazar Mrk 421 on year time scales, which can bring additional insight on the processes responsible for its broadband emission. We observed Mrk 421 in the very high energy gamma-ray range with the Cherenkov telescope MAGIC-I from March 2007 to June 2009. The 2.3-year long MAGIC light curve is complemented with data from the Swift/BAT and RXTE/ASM satellites and the KVA, GASP-WEBT, OVRO, and Metsahovi telescopes from February 2007 to July 2009, allowing for an excellent characterisation of the multi-band variability and correlations over year time scales.
10. Mrk 335 photometry in 1995-2004
ID:
ivo://CDS.VizieR/J/A+A/437/87
Title:
Mrk 335 photometry in 1995-2004
Short Name:
J/A+A/437/87
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present results of UBVRI photometry of Mrk 335 in 1995-2004. This object has a large amplitude of variability, reaching about 1.1, 0.9, 0.7mag in the U,B,V and 0.3mag in the Rc, Ic bands, respectively. ************************************************************************** * * * Sorry, but the author(s) never supplied the tabular material * * announced in the paper * * * **************************************************************************

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