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We present the results of a systematic search and analysis of GRBs detected by the Astrorivelatore Gamma ad Immagini LEggero (AGILE) MiniCALorimeter (MCAL; 0.4-100 MeV) over a time frame of 13 yr, from 2007 to 2020 November. The MCAL GRB sample consists of 503 bursts triggered by MCAL, 394 of which were fully detected onboard with high time resolution. The sample consists of about 44% short GRBs and 56% long GRBs. In addition, 109 bursts triggered partial MCAL onboard data acquisitions, providing further detections that can be used for joint analyses or triangulations. More than 90% of these GRBs were also detected by the AGILE Scientific RateMeters (RMs), providing simultaneous observations between 20 keV and 100 MeV. We performed spectral analysis of these events in the 0.4-50 MeV energy range. We could fit the time-integrated spectrum of 258 GRBs with a single power-law model, resulting in a mean photon index «β»of-2.3. Among them, 43 bursts could also be fitted with a Band model, with peak energy above 400 keV, resulting in a mean low-energy photon index «α» = -0.6, a mean high-energy photon index «β» = -2.5, and a mean peak energy «E p » = 640 keV. The AGILE MCAL GRB sample mostly consists of hard-spectrum GRBs, with a large fraction of short-duration events. We discuss properties and features of the MCAL bursts, whose detections can be used to perform joint broad-band analysis with other missions, and to provide insights on the high-energy component of the prompt emission in the tens of mega electron volt energy range.

Ten spectra of the quasar HE 0435-4312 taken at different dates with SALT telescope. Spectra are in the rest frame, corrected for the Galaxy extinction. The ten spectra are taken on 23 Dec 2012, 18 Feb 2013, 20 Aug 2013, 3 Feb 2014, 23 Aug 2014, 24 Nov 2014, 9 Jan 2015, 9 Aug 2015, 6 Oct 2015, 7 Dec 2015. (12 data files).

The Herschel/PACS 100 and 160um observations of HRS galaxies presented in this work have been obtained as part of various opentime Herschel projects.

(2 data files).

The complete sample presented in this paper consists of 104 northern and equatorial radio-loud AGN. It includes all AGN with declination >=-10° that have a measured average radio flux density at 37GHz exceeding 1Jy. Most of the sample sources have been monitored at Metsahovi Radio Observatory for many years, and the brightest sources have been observed for up to 30yr. (1 data file).

The XMM-LSS, XMM-CDFS, and XMM-COSMOS are three surveys with complementary properties in terms of luminosity and redshift coverage. We used these three surveys to derive Bayesian estimates of the unabsorbed luminosity function (LF) of AGN in the 2-10keV band. The LF estimates are presented as a set of samples from the posterior probability distribution of the LF parameters. The LF is parameterised as a double power-law, with either the luminosity and density evolution (LADE) model, or the luminosity-dependent density evolution (LDDE) model. The double power-law is described by Eq.(10) in the paper. The LADE and LDDE models are described by Eqs.(11-14) and Eqs.(15-17), respectively. A Fortran 2008 implementation of these models can be found in file src2/lumf_funcs.f90 of the LFTools package, in the classes doublepowerlaw, ladevol, and lddevol (see the paper).

(8 data files).

We release a data set to accompany the "First 3C279 Event Horizon Telescope Results" paper (Kim et al. 2020). The data set is derived from the Science Release 1 (SR1) of the Event Horizon Telescope (EHT)'s April 2017 observation campaign (EHTC et al. 2019ApJ...875L...3E).

This data set contains 3C279 data for both low and high bands for all observed days (April 5th, 6th, 10th, 11th, 2017). Data from the 2017 observations were processed through three independent reduction pipelines (Blackburn et al., 2019ApJ...882...23B, Janssen et al., 2019A&A...626A..75J, EHTC et al. 2019ApJ...875L...3E). This release includes the fringe fitted, a-priori calibrated, and network calibrated data from the EHT-HOPS pipeline, which is the primary data set for the First 3C279 EHT results. Independent flux calibration is performed based on estimated station sensitivities during the campaign (Issaoun et al., 2017, EHT Memo 2017-CE-02, Janssen et al. 2019A&A...626A..75J,). A description of the data properties, their validation, and estimated systematic errors is given in EHTC et al. (2019ApJ...875L...3E) with additional details in Wielgus et al. (2019, https://eventhorizontelescope.org/for-astronomers/memos).

The data are time averaged to 10 seconds and frequency averaged over all 32 intermediate frequencies (IFs). All polarization information is explicitly removed. To make the resulting 'uvfits' files compatible with popular very-long-baseline interferometry (VLBI) software packages, the circularly polarized cross-hand visibilities 'RL' and 'LR' are set to zero along with their errors, while parallel-hands 'RR' and 'LL' are both set to an estimated Stokes I value. Measurement errors for 'RR' and 'LL' are each set to sqrt(2) times the statistical errors for Stokes I.

All uvfits files are located in the "uvfits/" subdirectory. Easy-to-read csv and txt files are derived from the uvfits files and provided in "csv" and "txt", respectively. Scripts that generate these files from the original SR1 data are also included. Finally, the run.sh script in the top directory will convert uvfits files into csv and txt files.

The three tgz files are gzipped tarballs that contains uvfits, txt, and csv files, respectively. They are included in this repository for convenience.

(10 data files).

We used a recent dataset obtained on June 26th, 2019, as part of the LOFAR Two-metre Sky Survey (LoTSS, see Shimwell et al., 2019A&A...622A...1S, Cat. J/A+A/622/A1).

We observed the source with the Very Large Array (VLA) in A configuration on July 28th 2015 using the P-band receiver centered at 350MHz.

We reprocessed the data used by Roettiger et al. (1994ApJ...421L..23R) at 1400MHz and 4850MHz. The data consists of observations in B array at 1400MHz and in C array at 4850MHz. The target was observed for 7 hours at 1400MHz and for 5 hours at 4850MHz.

The target was observed with the legacy Giant Metrewave Radio Telescope (GMRT) at 614MHz and 240MHz in dual frequency mode and data were published in Lal et al. (2008MNRAS.390.1105L). The observations were performed on July 29th and 30th, 2005.

3C388 was observed by Chandra on February 9th and 29th, 2004 with the ACIS-I detector (obs ID 4756 and 5295, respectively) and the data were published by Kraft et al. (2006ApJ...639..753K).

(2 data files).

This paper presents the EPTA data set, up to mid-2014, that was gathered from the 'historical' pulsar instrumentations at EFF, JBO, NRT and WSRT with, respectively, the EBPP (Effelsberg-Berkeley Pulsar Processor), DFB (Digital FilterBank), BON (Berkeley-Orleans-Nancay) and PuMa (Pulsar Machine) backends. The data recorded with the newest generation of instrumentations, e.g. PSRIX at EFF (Lazarus et al., 2016MNRAS.458..868L) and PuMaII at WSRT (Karuppusamy, Stappers & van Straten 2008PASP..120..191K), will be part of a future EPTA data release. (8 data files).

One fits file for each spectrum of 51 Eridani b (SPHERE IFS-YJ, IFS-YH, Samland et al., 2017, this work; GPI-H band, Macintosh et al., 2015, Cat. J/other/Sci/350.64). The first extension of the file contains the spectrum used in the paper (fits-table). The second extension contains the correlation matrix for the uncertainty of the spectral points (fits-image). The petitCODE (a self-consistent 1d radiative-convective equilibrium code, see Molliere et al., 2015ApJ...813...47M, 2017A&A...600A..10M) atmospheric model grids (cloudy and clear) as used and described in Samland et al. 2017, this work, are provided as fits-files. The first extension contains the wavelength sampling of the model cube at a resolution of 1000 (same for all models). The second extension contains the table of all model parameter combinations (each row one model, columns represent parameters). The third extension contains the flattened model cube as 2D-fits image (index of row of table in 2nd ext. corresponds to index of model in 3rd extension). The header of the 3rd extension gives the dimensions of the model cube prior to flattening to make it easy to restore the non-flattened shape if necessary. Units and descriptions can always be found in the respective headers. (2 data files).

We used the Sextractor photometric catalogue of WINGS galaxies described in Varela et al. (2009A&A...497..667V, Cat. J/A+A/497/667), which refers to optical (B,V) photometry of 76 cluster of galaxies, either observed with the INT telescope at La Palma, or with the 2.2m ESO telescope at La Silla.

(1 data file).

Here we report an all-sky soft gamma-ray source catalog based on IBIS observations performed during the first 1000 orbits of INTEGRAL. The database for the construction of the source list consists of all good-quality data available, from the launch in 2002, up to the end of 2010. This corresponds to ~110Ms of scientific public observations, with a concentrated coverage on the Galactic Plane and extragalactic deep exposures. This new catalog includes 939 sources above a 4.5σ significance threshold detected in the 17-100keV energy band, of which 120 sources represent previously undiscovered soft gamma-ray emitters. The source positions are determined, mean fluxes are provided in two main energy bands, and these are both reported together with the overall source exposure. Indicative levels of variability are provided, and outburst times and durations are given for transient sources. A comparison is made with previous IBIS catalogs and catalogs from other similar missions. (2 data files).

We obtained 98 spectra of HD219134 using the HARPS-N spectrograph. Our RV data are provided online. spitzer.dat contains the photometric time-series presented in the paper for HD219134 and gathered by the IRAC instrument aboard the Spitzer telescope in its channel 2 (4.5 microns) on 2015-04-14.

The APOP is a absolute proper motion catalog achieved on the Digitized Sky Survey Schmidt plates data established by GSC-II project that outside the galactic plane (|b|>27°). The sky cover of this catalog is 22,525 square degree, the mean density is 4473 objects/sq.deg. and the magnitude limit is around R=20.8mag. The systematic errors of absolute proper motions related to the position, magnitude and color are practically all removed by using the extragalactic objects. The zero point error of absolute proper motions is less than 0.6mas/yr, and the accuracy is better than 4.0mas/yr for objects bright than R=18.5, and rises to 9.0mas/yr for objects with magnitude 18.5We believe the catalog is reliable for operational applications and will be also fine for astrophysical research. But the user should use this catalog with that in mind, the accuracy condition is good for objects with Declination>-30 degree and is not very well for others, the reason is that the epoch difference is large for Declination>-30° (45 years) but South than that is only around 12 years. It is fine for statistical studies for objects with Declination<-30° that people could find and remove obviously incorrect entries. (1 data file).

We analyse both X-Shooter and UVES spectra acquired at the VLT. We used a traditional abundance analysis based on OSMARCS 1D Local Thermodynamic Equilibrium (LTE) model atmospheres and the TURBOSPECTRUM line formation code.(2 data files).

A total of 219 stars have been selected along the RGB and the red horizontal branch (RHB) from the ACS@HST and WFI@2.2m ESO catalogs presented in Paper I (Dalessandro et al. 2014ApJ...791L...4D).

The observations have been performed with the multiplex facility FLAMES@ESO-VLT in the UVES+GIRAFFE combined mode (PID:093.D-0618, PI:Dalessandro). The employed gratings are the UVES Red Arm CD#3 580, which covers the spectral range between ~4800 and ~6800Å with a spectral resolution of ~45000, and the GIRAFFE setups HR11 (5597-5840Å and R~24000) and HR13 (6120-6405Å and R~22000). (1 data file).

For a sample of 143 stars in M80 observed with FLAMES@VLT we give here: identifications, coordinates, BV magnitudes, heliocentric RV (table2). For members we also give: atmospheric parameters, [Fe/H] (table 3); [O/Fe], [Na/Fe], [Mg/Fe], [Al/Fe] (table 5); the alpha-elements Si, Ca, and Ti (table 6); the Fe-peak elements Sc, V, Cr, Mn, Co, Ni, Cu, and Zn (table 7); the n-capture elements Y, Zr, La, Ce, Pr, Nd, Sm, (table 8, only UVES stars); Ba (table 9). (7 data files).

For a sample of 43 stars in NGC 5634 observed with FLAMES@VLT we give here: identifications, coordinates, VIK magnitudes, heliocentric RV (table2). (1 data file).

ALLSMOG is an ESO Large Programme for the Atacama Pathfinder EXperiment (APEX, project no.: E-192.A-0359, principal investigator (PI): J. Wagg) targeting the CO(2-1) emission line (rest frequency, ν_CO(2-1)=230.538GHz) in 88 local, low-M* star-forming galaxies. The project was initially allocated 300h of ESO observing time over the course of four semesters, corresponding to 75h per semester throughout periods P92-P95 (October 2013 - September 2015). However, during P94 and P95 there was a slowdown in ALLSMOG observations, mainly due the installation of the visiting instrument Supercam in combination with better-than-average weather conditions - causing other programmes requiring more stringent precipitable water vapour (PWV) constraints to be prioritised. Because of the resulting ~50% time loss for ALLSMOG during two semesters, the ESO observing programmes committee (OPC) granted a one-semester extension of the project, hence allowing us to complete the survey in P96 (March 2016). The final total APEX observing time dedicated to ALLSMOG amounts to 327h, including the overheads due to setup and calibration but not accounting for possible additional time lost because of technical issues.

In 2014 a northern component of the ALLSMOG survey was approved at the IRAM 30m telescope (project code: 188-14, PI: S. Martin), aimed at observing the CO(1-0) (rest frequency, ν_CO(1-0)=115.271GHz) and CO(2-1) emission lines in a sample of nine additional galaxies characterised by stellar masses, M*<10⁹M_ȯ. A total of 22h of observations were obtained with the IRAM 30m during two observing runs in November 2014 and May 2015.

(5 data files).

In this study we undertake a multi-wavelength analysis of the ALMA-detected submm galaxies from the catalog presented by Hodge et al. (2013, J/ApJ/768/91) (see also Karim et al. 2013MNRAS.432....2K). To briefly summarize the observations, we obtained 120 s integrations of 122 of the original 126 LESS submm sources, initially identified using the LABOCA camera on the APEX telescope (Weiss et al. 2009, J/ApJ/707/1201). These Cycle 0 observations used the compact configuration, yielding a median synthesized beam of ~1.6"x1.2". The observing frequency was matched to the original LESS survey, 344 GHz (Band 7), and we reach a typical rms across our velocity-integrated maps of 0.4 mJy/beam. (3 data files).

(ATESP) survey for a complete sub-sample of Optical/IR Multi-band selected early-type radio galaxies are displayed in the ASCII table. The original survey data at 1.4 and 5GHz were published in Prandoni et al. (2000A&AS..146...41P, Cat. VIII/63) and Prandoni et al. (2006, Cat. J/A+A/457/517). A higher frequency follow-up at 5, 8 and 19 GHz was presented in Prandoni et al. (2010A&A...510A..42P). The flux densities of the 28 souces making up the early-type complete sub-sample observed in Sep 2011 and July 2012 follow-up campaigns with the Australia Telescope Compact Array (ATCA) at the radio frequencies of 19, 38 and 94 GHz are presented in the ASCII table. 2011 38-GHz flux densities are showed both at high- (HR: 0.6 arcsec) and low- (LR: 10-15 arcsec) angular resolutions.