Herschel ivo://esavo/hsa/tap European Space Agency Bruno Merin esdc_leads@cosmos.esa.int +34918131456 ESA, Herschel, Archive, ESAC This service provides access to observations and catalogs from the ESA Herschel Space Observatory mission hosted at the ESAC Science Data Centre https://archives.esac.esa.int/hsa/whsa https://archives.esac.esa.int/hsa/whsa-tap-server/tap ADQL 2.0 ADQL 2.0 application/x-votable+xml votable application/x-votable+xml votable_plain text/csv csv application/json json application/fits fits text/plain direct 259200 259200 300 300 100000 100000 https://archives.esac.esa.int/hsa/whsa-tap-server/tap/capabilities https://archives.esac.esa.int/hsa/whsa-tap-server/tap/tables > tap_upload hpdp hpdp.latest_observation_hpdp file_oid INTEGER instrument_oid INTEGER observation_id VARCHAR request_oid INTEGER hpdp.vizier_links hpdp.unique_observation_hpdp aor VARCHAR category VARCHAR dec DOUBLE duration DOUBLE end_time TIMESTAMP fov VARCHAR instrument_oid INTEGER is_public BOOLEAN keyword VARCHAR naif_id VARCHAR num_requests BIGINT observation_id VARCHAR observation_oid INTEGER observer VARCHAR observing_mode_oid INTEGER obsstate VARCHAR od_number BIGINT polygon_fov VARCHAR prop_end TIMESTAMP proposal_id VARCHAR ra DOUBLE request_oid INTEGER spg_id VARCHAR start_time TIMESTAMP status VARCHAR target_name VARCHAR urn_version INTEGER hpdp.latest_unique_observation_requests instrument_oid INTEGER max_request_oid INTEGER num_requests BIGINT observation_id VARCHAR hpdp.files filename VARCHAR file_oid INTEGER file_size BIGINT file_type_oid INTEGER main_postcard BOOLEAN request_oid INTEGER vizier_link VARCHAR hpdp.latest_requests abstract text author text category VARCHAR date_active_version TIMESTAMP date_ingest_completed TIMESTAMP date_ingest_requested TIMESTAMP date_ingest_started TIMESTAMP directory VARCHAR full_retrieval_file_size BIGINT full_retrieval_path VARCHAR is_active_version BOOLEAN job_id VARCHAR keyword VARCHAR rel_notes_file VARCHAR request_file VARCHAR request_oid INTEGER title text version_change_log VARCHAR version_number INTEGER public public.dual auxiliary table to be used as dummy "from" dummy INTEGER public.image_formats extension VARCHAR image_format_oid INTEGER tap_schema tap_schema.tables TAP SCHEMA tables db_table_name VARCHAR description VARCHAR schema_name VARCHAR size BIGINT table_name VARCHAR table_type VARCHAR utype VARCHAR tap_schema.columns TAP SCHEMA columns column_name VARCHAR datatype VARCHAR db_column_name VARCHAR description VARCHAR indexed INTEGER principal INTEGER schema_name VARCHAR size INTEGER std INTEGER table_name VARCHAR ucd VARCHAR unit VARCHAR utype VARCHAR tap_schema.keys TAP SCHEMA keys description VARCHAR from_table VARCHAR key_id VARCHAR target_table VARCHAR utype VARCHAR tap_schema.schemas TAP SCHEMA schemas db_schema_name VARCHAR description VARCHAR schema_name VARCHAR utype VARCHAR tap_schema.key_columns TAP SCHEMA key columns from_column VARCHAR key_id VARCHAR target_column VARCHAR hsa hsa.observation_science global_science_area VARCHAR instrument_name VARCHAR instrument_oid INTEGER observation_id VARCHAR observation_science_oid INTEGER science_area VARCHAR science_category VARCHAR hsa.proposal_coauthor coauthor VARCHAR coauthor_short_name VARCHAR coauthor_short_name_plain VARCHAR proposal_coauthor_oid INTEGER proposal_id VARCHAR hsa.proposal_observation observation_oid INTEGER proposal_observation_oid INTEGER proposal_oid INTEGER hsa.instrument instrument_name VARCHAR instrument_oid INTEGER hsa.observing_mode_per_instrument hsa.spire_spectral_feature_finder_catalogue obsid The OBSID meta.ref.url Acess.reference VARCHAR primary opday The Herschel Operational Day INTEGER primary frequency Observed frequency of the feature GHz DOUBLE primary frequency_error Error on the derived frequency GHz DOUBLE primary rest_frame_freq Rest-frame frequency of the feature GHz DOUBLE primary snr Signal-to-noise ratio DOUBLE primary detector_array Detector or detector array name VARCHAR primary cube_pixel_row Cube pixel row INTEGER primary cube_pixel_column Cube pixel column INTEGER primary ra The Right Ascension J2000.0 deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE primary dec The Declination J2000.0 deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE primary feature_flag Combined flag for the feature DOUBLE primary velocity The derived radial velocity km/s DOUBLE primary velocity_error Radial velocity error km/s DOUBLE primary v_flag Radial velocity flag VARCHAR primary extent Point-like or extended source VARCHAR primary calibration Point-like or extended source calibration used for the feature VARCHAR primary sampling Map sampling VARCHAR primary hpdp HPDP products used INTEGER primary bgs Background subtracted spectra used INTEGER primary ncc_flag Special search for [CI] feature INTEGER primary hsa.hifi_spectral_line_smoothed obsid Observation ID meta.ref.url Acess.reference VARCHAR primary source_id Name of the source VARCHAR primary ra Right Ascension coordinate deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE primary dec Declination coordinate deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE primary observing_mode HIFI Observing mode name VARCHAR primary spectrograph Name of spectrometer backend. Save for a handful of exceptions, it will always be "WBS-HV" as both polarisations should have been averaged to form the input spectrum VARCHAR primary spectra_resolution Spectral resolution of input spectrum. For the default LineCatalogue, this corresponds to the native resolution (around 1 MHz), while for smoothed tables, it indicates the resulting spectral bin size after smoothing MHz DOUBLE primary database Data-base from which the line spectroscopy parameters are taken (JPLor CDMS) VARCHAR primary species Name of the molecular or atomic species VARCHAR primary transition Name of transition VARCHAR primary rest_frequency Frequency of the line transition in the LSR GHz DOUBLE primary eup Upper energy level Eup of the line K DOUBLE primary aij Einstein coefficient Aij 1/s DOUBLE primary position Fitted position of the line centroid GHz DOUBLE primary std_position Standard deviation error on the above fitted position GHz DOUBLE primary side_band Name of the sideband frequency scale (here "SSB", i.e. Single Side-band) VARCHAR primary v0 Position of the velocity centroid km/s DOUBLE primary std_v0 Standard deviation error on the fitted centroid km/s DOUBLE primary rms RMS noise level of the spectra estimated from the spectrum on two windows of 50 MHz on either side of the line profile K DOUBLE primary signal_to_noise_ratio Fitted line peak signal-to-noise ratio DOUBLE primary evidence Provides a quality measure of the Gaussian fit (based on a Bayesianstatistics fitter) DOUBLE primary peak_position Frequency position of the fitted line peak (GHz) GHz DOUBLE primary lower_frequency_fit_window Lower frequency of the interval used to perform the Gaussian fit(GHz) GHz DOUBLE primary upper_frequency_fit_window Higher frequency of the interval used to perform the Gaussian fit(GHz) GHz DOUBLE primary hsa.publication author VARCHAR bib_code VARCHAR instrument_name VARCHAR observation_id VARCHAR publication_oid INTEGER title VARCHAR hsa.quality_flag flag_action text flag_description text flag_impact text flag_name VARCHAR flag_value VARCHAR observation_oid INTEGER quality_flag_oid INTEGER hsa.v_active_observation aor AOR label as entered in HSPOT VARCHAR bii Galactic longitude in degrees DOUBLE dec Actual declination of pointing deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE duration Duration of the observation in seconds DOUBLE end_time End date of the observation TIMESTAMP fov Field of view VARCHAR global_science_area HSA internal parameter VARCHAR icon_image HSA internal parameter BINARY icon_location HSA internal parameter VARCHAR image_2_5_location HSA internal parameter VARCHAR image_location HSA internal parameter VARCHAR ingest_queue_oid Database index number INTEGER instrument_oid Database index number INTEGER is_active_version HSA internal parameter BOOLEAN is_public Is the observation public or restricted BOOLEAN lii Galactic latitude in degrees DOUBLE naif_id Solar sytem objects identifier VARCHAR num_publications BIGINT observation_id The identifier of a Herschel observation VARCHAR observation_oid Database index number INTEGER observer Name of the principal investigator of the observation VARCHAR observing_mode_oid Database index number INTEGER obsstate Final status of the observation after QC assessment: PASSED, FAILED, NOT APPLICABLE VARCHAR od_number The operational day to which the observation belongs BIGINT pa Position angle of pointing DOUBLE polygon_fov HSA internal parameter VARCHAR position HSA internal parameter VARCHAR prop_end HSA internal parameter TIMESTAMP proposal_id The ID of the proposal that the observation was part of VARCHAR quality_report_location HSA internal parameter VARCHAR ra Actual right ascension of pointing deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE science_area Broad Science Area classification of the observations as entered by the user in HSpot: Galactic, Extra-galactic, Solar System. VARCHAR science_category Detailed Science Category classification of the observations as entered by the user in HSpot. VARCHAR spg_id Version of the Pipeline used to process the obervation VARCHAR start_time Start date of the observation TIMESTAMP status Access status: Public or Restricted VARCHAR target_name The name of the target VARCHAR urn_version HSA internal parameter INTEGER hsa.proposal_info abstract VARCHAR author VARCHAR author_plain VARCHAR proposal_id VARCHAR proposal_info_oid INTEGER title VARCHAR hsa.pacs_point_source_070 source_id The object name is an identifier consisting of two parts, acronym and sequence, and is formatted as ’HPPSCxxxA_Jhhmmss.s±ddmmss’. ’HPPSC’ stands for Herschel PACS Point Source Catalogue, xxx is the central wavelength of the band in which the source was observed, identifying the wavelength in microns, and the letter A indicates the first version of the catalogue. The second part has the format ’Jhhmmss.s+ddmmss’ derived from the source coordinates with ’J’ indicating a J2000 reference system, ’hhmmss.s’ is the Right Ascension in hours, minutes and seconds accuracy of one digits after the decimal, and ’+ddmmss’ is the Declination in signed degrees, minutes and seconds to an accuracy of one digit after the decimal. VARCHAR primary band This is one of the strings "blue","green","red" identifying the PACS detector array names for the filter bands centred at 70, 100, 160 microns, respectively. The wavelength is also specified in the name of the object. microns VARCHAR primary ra Right Ascension coordinate in a J2000.0 reference frame. This is the peak position of the SUSSEXtractor detection. The coordinates are degrees written in double precision format. deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE primary dec Declination coordinate in a J2000.0 reference frame. This is the peak position of the SUSSEXtractor detection. The coordinates are degrees written in double precision format. deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE primary raerr Positional uncertainties of each object as provided by SUSSEXtractor. Units are degrees, the data type is double precision. deg DOUBLE primary decerr Positional uncertainties of each object as provided by SUSSEXtractor. Units are degrees, the data type is double precision. deg DOUBLE primary flux This is the flux as provided by the AnnularSkyAperturePhotometry task. For objects that were identified several times across different maps, this flux corresponds to the extraction with the best average S/N, where the Ns based S/N (S/Ns)and the background RMS based S/N (S/Nr) values are taken into account. For the blue and green bands the aperture radius was 6??, for the red band 12?? (see Section 3.3 for more details). For all cases the raw flux density values were corrected for the aperture size, based on Lutz (2015). Colour corrections were not applied. The units are mJy, written as double precision. mJy DOUBLE primary snr Estimated S/N based on a statistical approach, using the S/Ns calibration surfaces. It is calculated as a function of the source flux and the Ns value. The data type is double precision. DOUBLE primary snrnoise It is calculated from the source flux and the estimated S/Ns, by dividing the flux by the S/Ns. This noise includes both the sky confusion and the instrument noise. DOUBLE primary stn Calculated as the ratio of the source flux and the RMS. Data type is double precision. DOUBLE primary rms RMS noise as measured in the blank sky apertures placed around the source. Double precision. Units are mJy. mJy DOUBLE primary strn Structure noise value obtained from the structure noise maps. Double precision, in units of MJy/sr. MJy/sr DOUBLE primary fratio The ratio of the flux density values measured in the 6th and the 1st aperture, corresponding to 4?? and 9?? in the blue and green bands, and 9?? and 14?? in the red band. DOUBLE primary fwhmxfit This column contains the FWHM values measured by the 2D Gaussian model in X and Y directions, fitted by the sourceFitter() task. If the elongated Gaussian fit was possible then both FWHMx and FWHMy are listed. If only a circular Gaussian could be fitted then FWHMy is equal to -99.9. It is written in double precision format, in units of second of arc. arcsec DOUBLE primary fwhmyfit This column contains the FWHM values measured by the 2D Gaussian model in X and Y directions, fitted by the sourceFitter() task. If the elongated Gaussian fit was possible then both FWHMx and FWHMy are listed. If only a circular Gaussian could be fitted then FWHMy is equal to -99.9. It is written in double precision format, in units of second of arc. arcsec DOUBLE primary elong_flag If an elliptical Gaussian model was fitted in the source, this column contains the ratio of the FWHMy and FWHMx. A value of 0 means that the source is circular, 0.5 means that FWHMy = 0.5 × FWHMx. If FWHMy = -99.9 (circular detection), FLAG_ELONG = 0. FLAG_ELONG is also set to 0 if the source eccentricity (FWHMx - FWHMy)/FWHMx) defined in a similar way with the FWHM values of the PACS PSF reported in Table 1, is smaller than the PSF eccentricity, Double precision format. DOUBLE primary edge_flag The position of a source with respect to the edges of the image affects the quality of the photometry, as the extraction procedure needs a large enough area to compute properly both the flux density and the background to be subtracted. Also, due to the scan speed inhomogeneities during the turnarounds, the map edges may have different noise properties than the rest of the image. BOOLEAN primary blend_flag Objects with distance within the PSF FWHM have the same value (>0) of FLAG_BLEND and they can be considered as blended sources. FLAG_BLEND = 0 means that the object is not blended with other objects. The PACS PSFs depend on the observing mode. The absolute pointing error for SPG13 (1.2??) is adopted as uncertainty. DOUBLE primary warmat Flag indicating that the observation was affected by "warm" attitude. The term refers to spacecraft attitudes in which the star-tracker support structure is subject to thermal distortions as was not completely shaded from sunlight. This has an impact on the pointing accuracy. Data type is Boolean. BOOLEAN primary obsid The term is the observation identifier for the Herschel observations . It is a 10 digit integer, starting always with 1342. The column lists the first OBSID from the list that built the L2.5/L3 map. It corresponds to the meta keyword obsid001. meta.ref.url Acess.reference VARCHAR primary ssomap_flag Maps of solar system objects have typically been observed in tracking mode, but were reprocessed in the ’rest’ sky frame for the HPPSC, and may be contaminated by the moving targets. The affected OBSIDs are marked with an ’ssomap’ flag. BOOLEAN primary hsa.observing_mode observing_mode_name VARCHAR observing_mode_oid INTEGER search_key VARCHAR hsa.proposal angle_from VARCHAR angle_to VARCHAR aor VARCHAR band VARCHAR cross_step_size VARCHAR dec_j2000 VARCHAR dec_j2000_deg VARCHAR fov USER-DEFINED instrument VARCHAR is_time_constrained VARCHAR map_angle_ref VARCHAR map_position_angle VARCHAR map_radius VARCHAR map_x_size VARCHAR map_y_size VARCHAR mode VARCHAR naif_id VARCHAR nominal_ortogonal VARCHAR num_legs VARCHAR num_repetitions VARCHAR nyquist_sampling VARCHAR offset_true_false VARCHAR overhead_time VARCHAR proposal_id VARCHAR proposal_oid INTEGER ra_j2000 VARCHAR ra_j2000_deg VARCHAR raster_lines VARCHAR raster_point_line VARCHAR raster_x_step VARCHAR raster_y_step VARCHAR scan_cross_step VARCHAR scan_line_length VARCHAR scan_map_cross_size VARCHAR scan_speed VARCHAR spectrometer VARCHAR submode VARCHAR target_name VARCHAR target_type VARCHAR total_time VARCHAR hsa.proposal_pi_user proposal_oid INTEGER proposal_pi_user_oid INTEGER short_name VARCHAR short_name_plain VARCHAR username VARCHAR hsa.spire_point_source_350 source_id The object identifier consists of two parts, acronym and sequence, and is formatted as “HSPSCwwwA_Jhhmm.mm+ddmm.m” with the exception of the planets Uranus and Neptune, which are following the format “HSPSCwwwA_ppp_000”. “HSPSC” stands for Herschel SPIRE Point Source Catalog, “www” is one of [250,350,500], identifying the wavelength in microns, and the letter A indicates the first public version of the catalog. The sequence has the format “Jhhmm.mm+ddmm.m”, which is derived from the object coordinates with J indicating a J2000 reference system, “hhmm.mm” indicating the Right Ascension in hours and minutes to an accuracy of two digits after the decimal, and “+ddmm.m” indicating Declination in signed degrees and minutes to an accuracy of one digit after the decimal. In the case of the planets the sequence is formatted as “ppp_000”, where “ppp” stands for one of the strings “URA” or “NEP” indicating Uranus or Neptune respectively, followed by a running number “000” indicating the observation. The spatial resolution of the coordinate based serial number is well matched to the size of SPIRE’s beam profiles and will keep changes in object names to a minimum if another version of the catalog is generated. VARCHAR primary det This is one of the strings “PSW”, “PMW”, “PLW” identifying the SPIRE detector array names for the filter bands centered at 250, 350, 500 microns respectively. This column is for convenience for those more familiar with the instrument specific naming. Otherwise the wavelength is indicated in the object identifier. VARCHAR primary ra Right Ascension coordinate in a J2000.0 reference frame, calculated as the average of the Right Ascensions of all the contributing source detections in different maps. The positions used result from the refined Timeline Fitter positions and their uncertainties. The average is calculated in Cartesian space and transformed back to spherical coordinates to avoid problems near the celestial poles. deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE primary dec Declination coordinate in a J2000.0 reference frame, calculated as the average of the Right Ascensions of all the contributing source detections in different maps. The positions used result from the refined Timeline Fitter positions and their uncertainties. The average is calculated in Cartesian space and transformed back to spherical coordinates to avoid problems near the celestial poles. deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE primary ra_err Positional uncertainty in arcsec of each catalog object. It is derived as the larger of either quadratic mean of all the individual TML uncertainties of all contributing source detections or the standard deviation of all source positions, divided by the square root of the number of maps the source is detected in. arcsec DOUBLE primary dec_err Positional uncertainty in arcsec of each catalog object. It is derived as the larger of either quadratic mean of all the individual TML uncertainties of all contributing source detections or the standard deviation of all source positions, divided by the square root of the number of maps the source is detected in. arcsec DOUBLE primary pos_flag This flag indicates a potential problem with the position of this source if set to True. It is set if the uncertainties associated with the position are larger than the search radius used by the consolidation algorithm. It is also set if the maximum distance between the positions of all contributing detections is larger than the search radius used by the consolidation algorithm. The search radius is chosen as half of the FWHM of the beam profile for the respective source increased by 6” as allowance for the 3 sigma pointing uncertainty of Herschel VARCHAR primary astrom_flag Astrometry flag indicating that one or more of the contributing source detections came from a map with a positional offset greater than 5” derived from stacking at WISE 24 ?m catalog positions. A total of 140573 records was flagged in this way. VARCHAR primary nmap The number of times a source should have been detected at the list position and in the same band pass, based on the coverage maps. This value is derived by testing a 3x3 pixel square centered on the source in each coverage map. If the coverage anywhere within this square is greater than zero, the NMAP value for this object is incremented by one. INTEGER primary ndet This column contains the actual number of detections in separate maps of this object at this position and filter band. Combinations of maps into a Level 2.5 map are counted as one. There are rare cases where two close, but separate detections in the same map become part of the same object because the grouping algorithm was not able to distinguish them. In this case the source duplication flag is set. INTEGER primary dupl_flag This flag is False by default and set to True if more than one source from the same map were identified as part of this object by the object consolidation algorithm. This is a rare occurrence and mainly due to limitations of the algorithm used. The flag was set 1624 times (960,497,167 for the filter bands respectively). VARCHAR primary flux This column shows the average of the TML derived fluxes of all contributing sources, weighted with the respective TML generated uncertainties. This procedure of fitting a fixed width circular Gaussian beam profile model has proven to be superior to a number of other common methods used with SPIRE data in terms of reproducibility and photometric accuracy, down to fluxes of 30 mJy (Pearson et al. 2014). mJy DOUBLE primary fluxtml_err This column contains the propagated weighted error produced by the TML for all contributing source detections. mJy DOUBLE primary conf_err This column indicates the local confusion uncertainty in mJy. It is the average of the individual values of all contributing sources, weighted with the respective TML uncertainties. mJy DOUBLE primary flux_err This column indicates the local confusion uncertainty in mJy. It is the average of the individual values of all contributing sources, weighted with the respective TML uncertainties. mJy DOUBLE primary snr This value has been added for convenience and expresses the signal to noise ratio associated with a given object as the ratio between the Timeline Fitter flux (FLUX) and the total flux error (FLUX_ERR). DOUBLE primary insterr_flag This flag indicates that the TML returned no count for the number of readouts in the central aperture. To still be able to derive an instrument noise component, a typical number was used, based on the instrument configuration and multiplied with the number of repeats of the observation. VARCHAR primary fluxsus This column shows the average of the Sussextractor derived fluxes of all contributing sources, weighted with the respective Sussextractor generated uncertainties. mJy DOUBLE primary fluxsus_err This column contains the propagated weighted error produced by Sussextractor for all contributing source detections. mJy DOUBLE primary fluxdao This column shows the average of the Daophot derived fluxes of all contributing sources, weighted with the respective Daophot generated uncertainties. mJy DOUBLE primary fluxdao_err This column contains the propagated weighted error produced by Daophot for all contributing source detections. mJy DOUBLE primary fluxtm2 This column shows the average of the TM2 derived fluxes of all contributing sources, weighted with the respective TM2 generated uncertainties. This procedure fits an elliptical Gaussian beam profile model where the major and minor axes have been left as free fit parameters. The configuration also allows for a tilted background plane. mJy DOUBLE primary fluxtm2_err This column contains the propagated weighted error produced by TML2 for all contributing source detections. mJy DOUBLE primary fwhm1 This column contains the average FWHM of the major axes of the elliptical Gaussian beam profile models fitted during the TM2 run to all the contributing detections, weighted by their respective uncertainties. arcsec DOUBLE primary fwhm2 This column contains the average FWHM of the minor axes of the elliptical Gaussian beam profile models fitted during the TM2 run to all the contributing detections, weighted by their respective uncertainties. arcsec DOUBLE primary fwhm1_err This column contains the respective uncertainties of the weighted averages of the major and minor axes of the fitted elliptical Gaussian beam profile in arcsec. arcsec DOUBLE primary fwhm2_err This column contains the respective uncertainties of the weighted averages of the major and minor axes of the fitted elliptical Gaussian beam profile in arcsec. arcsec DOUBLE primary rot This column contains a robust average rotation angle of the elliptical Gaussian beam profile models fitted during the TM2 run to all the contributing detections. Robust meaning that all angles with uncertainties that are larger than a factor 1.5 of the median of all uncertainties of the contributing detections are removed before averaging. The rotation angle on the sky is measured from West counter-clockwise in degrees. Possible values start from 0 and are smaller than 180 deg. The average of the angles is calculated in Cartesian space to avoid problems when crossing the 180 deg threshold. Since a position angle of 180 deg is equal to 0 deg, we multiplied the position angles by 2 before averaging and divided by 2 after the back-transformation. A constant of 180 deg was added when the angle was smaller than 0 to stay within the allowed range. dec DOUBLE primary rot_err This column contains the propagated error of the rotation angle for all contributing source detections. dec DOUBLE primary pntsrc_flag The flag is set for all objects, where both the major and minor FWHM parameters are still compatible with values that are observed from point sources at a given flux level. As such it is an indicator but not conclusive, in particular not for small fluxes. VARCHAR primary extsrc_flag This flag is set if any of the major or minor FWHM is larger than the upper flux dependent threshold for point sources. VARCHAR primary lowfwhm_flag This flag is set if any of the major or minor FWHM is smaller than the lower flux dependent threshold for point sources. VARCHAR primary largegal_flag This flag is set when the catalog position is within one of the ellipses given in the 2MASS Large Galaxy Atlas (LGA) (Jarrett et al 2003) for galaxies with major axis > 1arcmin. The values are described as 'K_s (LGA/2MASS "total")' and represent the standard 2MASS aperture. If the flag is set there is a high probability that the source is part of the respective large galaxy rather than a background object. VARCHAR primary mapedge_flag The map edge flag is set when at least one of the contributing sources shows 10 or more percent of map pixels without a flux value (NaN) within the outer radius of the background annulus used by the Timeline Fitter (74”, 103”, 147”) for 250, 350, and 500 microns respectively. This condition flags catalog objects where its detection or the flux estimate may have been affected by at least one contributor being close to a map edge. 24313 objects are the edge flag set. VARCHAR primary ssocont_flag This flag is set as a warning if any of the known contributors to the catalog object is within a rectangle defined by the tracklet of a known asteroid at the time of the observation of the respective map, and the beam FWHM at the wavelength of the map. The estimated flux using a simple asteroid standard model needs to be at least at the one sigma confusion limit of Nguyen et al. (2010) of 5.8, 6.3, 6.8 mJy for 250, 350, and 500 microns respectively. 810 objects have this flag set. VARCHAR primary q3ctile As the exclusion criterion for regions with highly structured background emission is determined on the basis of the median STRN within a Q3C tile at the 22 bit level, we add the respective Q3C tile identifier to each object. It is a 19 digit number that is best interpreted using the Postgres implementation of Q3C. DOUBLE primary hsa.spire_point_source_250 source_id The object identifier consists of two parts, acronym and sequence, and is formatted as “HSPSCwwwA_Jhhmm.mm+ddmm.m” with the exception of the planets Uranus and Neptune, which are following the format “HSPSCwwwA_ppp_000”. “HSPSC” stands for Herschel SPIRE Point Source Catalog, “www” is one of [250,350,500], identifying the wavelength in microns, and the letter A indicates the first public version of the catalog. The sequence has the format “Jhhmm.mm+ddmm.m”, which is derived from the object coordinates with J indicating a J2000 reference system, “hhmm.mm” indicating the Right Ascension in hours and minutes to an accuracy of two digits after the decimal, and “+ddmm.m” indicating Declination in signed degrees and minutes to an accuracy of one digit after the decimal. In the case of the planets the sequence is formatted as “ppp_000”, where “ppp” stands for one of the strings “URA” or “NEP” indicating Uranus or Neptune respectively, followed by a running number “000” indicating the observation. The spatial resolution of the coordinate based serial number is well matched to the size of SPIRE’s beam profiles and will keep changes in object names to a minimum if another version of the catalog is generated. VARCHAR primary det This is one of the strings “PSW”, “PMW”, “PLW” identifying the SPIRE detector array names for the filter bands centered at 250, 350, 500 microns respectively. This column is for convenience for those more familiar with the instrument specific naming. Otherwise the wavelength is indicated in the object identifier. VARCHAR primary ra Right Ascension coordinate in a J2000.0 reference frame, calculated as the average of the Right Ascensions of all the contributing source detections in different maps. The positions used result from the refined Timeline Fitter positions and their uncertainties. The average is calculated in Cartesian space and transformed back to spherical coordinates to avoid problems near the celestial poles. deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE primary dec Declination coordinate in a J2000.0 reference frame, calculated as the average of the Right Ascensions of all the contributing source detections in different maps. The positions used result from the refined Timeline Fitter positions and their uncertainties. The average is calculated in Cartesian space and transformed back to spherical coordinates to avoid problems near the celestial poles. deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE primary ra_err Positional uncertainty in arcsec of each catalog object. It is derived as the larger of either quadratic mean of all the individual TML uncertainties of all contributing source detections or the standard deviation of all source positions, divided by the square root of the number of maps the source is detected in. arcsec DOUBLE primary dec_err Positional uncertainty in arcsec of each catalog object. It is derived as the larger of either quadratic mean of all the individual TML uncertainties of all contributing source detections or the standard deviation of all source positions, divided by the square root of the number of maps the source is detected in. arcsec DOUBLE primary pos_flag This flag indicates a potential problem with the position of this source if set to True. It is set if the uncertainties associated with the position are larger than the search radius used by the consolidation algorithm. It is also set if the maximum distance between the positions of all contributing detections is larger than the search radius used by the consolidation algorithm. The search radius is chosen as half of the FWHM of the beam profile for the respective source increased by 6” as allowance for the 3 sigma pointing uncertainty of Herschel VARCHAR primary astrom_flag Astrometry flag indicating that one or more of the contributing source detections came from a map with a positional offset greater than 5” derived from stacking at WISE 24 ?m catalog positions. A total of 140573 records was flagged in this way. VARCHAR primary nmap The number of times a source should have been detected at the list position and in the same band pass, based on the coverage maps. This value is derived by testing a 3x3 pixel square centered on the source in each coverage map. If the coverage anywhere within this square is greater than zero, the NMAP value for this object is incremented by one. INTEGER primary ndet This column contains the actual number of detections in separate maps of this object at this position and filter band. Combinations of maps into a Level 2.5 map are counted as one. There are rare cases where two close, but separate detections in the same map become part of the same object because the grouping algorithm was not able to distinguish them. In this case the source duplication flag is set. INTEGER primary dupl_flag This flag is False by default and set to True if more than one source from the same map were identified as part of this object by the object consolidation algorithm. This is a rare occurrence and mainly due to limitations of the algorithm used. The flag was set 1624 times (960,497,167 for the filter bands respectively). VARCHAR primary flux This column shows the average of the TML derived fluxes of all contributing sources, weighted with the respective TML generated uncertainties. This procedure of fitting a fixed width circular Gaussian beam profile model has proven to be superior to a number of other common methods used with SPIRE data in terms of reproducibility and photometric accuracy, down to fluxes of 30 mJy (Pearson et al. 2014). mJy DOUBLE primary fluxtml_err This column contains the propagated weighted error produced by the TML for all contributing source detections. mJy DOUBLE primary conf_err This column indicates the local confusion uncertainty in mJy. It is the average of the individual values of all contributing sources, weighted with the respective TML uncertainties. mJy DOUBLE primary flux_err This column indicates the local confusion uncertainty in mJy. It is the average of the individual values of all contributing sources, weighted with the respective TML uncertainties. mJy DOUBLE primary snr This value has been added for convenience and expresses the signal to noise ratio associated with a given object as the ratio between the Timeline Fitter flux (FLUX) and the total flux error (FLUX_ERR). DOUBLE primary insterr_flag This flag indicates that the TML returned no count for the number of readouts in the central aperture. To still be able to derive an instrument noise component, a typical number was used, based on the instrument configuration and multiplied with the number of repeats of the observation. VARCHAR primary fluxsus This column shows the average of the Sussextractor derived fluxes of all contributing sources, weighted with the respective Sussextractor generated uncertainties. mJy DOUBLE primary fluxsus_err This column contains the propagated weighted error produced by Sussextractor for all contributing source detections. mJy DOUBLE primary fluxdao This column shows the average of the Daophot derived fluxes of all contributing sources, weighted with the respective Daophot generated uncertainties. mJy DOUBLE primary fluxdao_err This column contains the propagated weighted error produced by Daophot for all contributing source detections. mJy DOUBLE primary fluxtm2 This column shows the average of the TM2 derived fluxes of all contributing sources, weighted with the respective TM2 generated uncertainties. This procedure fits an elliptical Gaussian beam profile model where the major and minor axes have been left as free fit parameters. The configuration also allows for a tilted background plane. mJy DOUBLE primary fluxtm2_err This column contains the propagated weighted error produced by TML2 for all contributing source detections. mJy DOUBLE primary fwhm1 This column contains the average FWHM of the major axes of the elliptical Gaussian beam profile models fitted during the TM2 run to all the contributing detections, weighted by their respective uncertainties. arcsec DOUBLE primary fwhm2 This column contains the average FWHM of the minor axes of the elliptical Gaussian beam profile models fitted during the TM2 run to all the contributing detections, weighted by their respective uncertainties. arcsec DOUBLE primary fwhm1_err This column contains the respective uncertainties of the weighted averages of the major and minor axes of the fitted elliptical Gaussian beam profile in arcsec. arcsec DOUBLE primary fwhm2_err This column contains the respective uncertainties of the weighted averages of the major and minor axes of the fitted elliptical Gaussian beam profile in arcsec. arcsec DOUBLE primary rot This column contains a robust average rotation angle of the elliptical Gaussian beam profile models fitted during the TM2 run to all the contributing detections. Robust meaning that all angles with uncertainties that are larger than a factor 1.5 of the median of all uncertainties of the contributing detections are removed before averaging. The rotation angle on the sky is measured from West counter-clockwise in degrees. Possible values start from 0 and are smaller than 180 deg. The average of the angles is calculated in Cartesian space to avoid problems when crossing the 180 deg threshold. Since a position angle of 180 deg is equal to 0 deg, we multiplied the position angles by 2 before averaging and divided by 2 after the back-transformation. A constant of 180 deg was added when the angle was smaller than 0 to stay within the allowed range. dec DOUBLE primary rot_err This column contains the propagated error of the rotation angle for all contributing source detections. dec DOUBLE primary pntsrc_flag The flag is set for all objects, where both the major and minor FWHM parameters are still compatible with values that are observed from point sources at a given flux level. As such it is an indicator but not conclusive, in particular not for small fluxes. VARCHAR primary extsrc_flag This flag is set if any of the major or minor FWHM is larger than the upper flux dependent threshold for point sources. VARCHAR primary lowfwhm_flag This flag is set if any of the major or minor FWHM is smaller than the lower flux dependent threshold for point sources. VARCHAR primary largegal_flag This flag is set when the catalog position is within one of the ellipses given in the 2MASS Large Galaxy Atlas (LGA) (Jarrett et al 2003) for galaxies with major axis > 1arcmin. The values are described as 'K_s (LGA/2MASS "total")' and represent the standard 2MASS aperture. If the flag is set there is a high probability that the source is part of the respective large galaxy rather than a background object. VARCHAR primary mapedge_flag The map edge flag is set when at least one of the contributing sources shows 10 or more percent of map pixels without a flux value (NaN) within the outer radius of the background annulus used by the Timeline Fitter (74”, 103”, 147”) for 250, 350, and 500 microns respectively. This condition flags catalog objects where its detection or the flux estimate may have been affected by at least one contributor being close to a map edge. 24313 objects are the edge flag set. VARCHAR primary ssocont_flag This flag is set as a warning if any of the known contributors to the catalog object is within a rectangle defined by the tracklet of a known asteroid at the time of the observation of the respective map, and the beam FWHM at the wavelength of the map. The estimated flux using a simple asteroid standard model needs to be at least at the one sigma confusion limit of Nguyen et al. (2010) of 5.8, 6.3, 6.8 mJy for 250, 350, and 500 microns respectively. 810 objects have this flag set. VARCHAR primary q3ctile As the exclusion criterion for regions with highly structured background emission is determined on the basis of the median STRN within a Q3C tile at the 22 bit level, we add the respective Q3C tile identifier to each object. It is a 19 digit number that is best interpreted using the Postgres implementation of Q3C. DOUBLE primary hsa.v_publication abstract VARCHAR authors VARCHAR bib_code VARCHAR instrument_name VARCHAR num_observations INTEGER observation_id VARCHAR title VARCHAR hsa.spire_point_source_500 source_id The object identifier consists of two parts, acronym and sequence, and is formatted as “HSPSCwwwA_Jhhmm.mm+ddmm.m” with the exception of the planets Uranus and Neptune, which are following the format “HSPSCwwwA_ppp_000”. “HSPSC” stands for Herschel SPIRE Point Source Catalog, “www” is one of [250,350,500], identifying the wavelength in microns, and the letter A indicates the first public version of the catalog. The sequence has the format “Jhhmm.mm+ddmm.m”, which is derived from the object coordinates with J indicating a J2000 reference system, “hhmm.mm” indicating the Right Ascension in hours and minutes to an accuracy of two digits after the decimal, and “+ddmm.m” indicating Declination in signed degrees and minutes to an accuracy of one digit after the decimal. In the case of the planets the sequence is formatted as “ppp_000”, where “ppp” stands for one of the strings “URA” or “NEP” indicating Uranus or Neptune respectively, followed by a running number “000” indicating the observation. The spatial resolution of the coordinate based serial number is well matched to the size of SPIRE’s beam profiles and will keep changes in object names to a minimum if another version of the catalog is generated. VARCHAR primary det This is one of the strings “PSW”, “PMW”, “PLW” identifying the SPIRE detector array names for the filter bands centered at 250, 350, 500 microns respectively. This column is for convenience for those more familiar with the instrument specific naming. Otherwise the wavelength is indicated in the object identifier. VARCHAR primary ra Right Ascension coordinate in a J2000.0 reference frame, calculated as the average of the Right Ascensions of all the contributing source detections in different maps. The positions used result from the refined Timeline Fitter positions and their uncertainties. The average is calculated in Cartesian space and transformed back to spherical coordinates to avoid problems near the celestial poles. deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE primary dec Declination coordinate in a J2000.0 reference frame, calculated as the average of the Right Ascensions of all the contributing source detections in different maps. The positions used result from the refined Timeline Fitter positions and their uncertainties. The average is calculated in Cartesian space and transformed back to spherical coordinates to avoid problems near the celestial poles. deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE primary ra_err Positional uncertainty in arcsec of each catalog object. It is derived as the larger of either quadratic mean of all the individual TML uncertainties of all contributing source detections or the standard deviation of all source positions, divided by the square root of the number of maps the source is detected in. arcsec DOUBLE primary dec_err Positional uncertainty in arcsec of each catalog object. It is derived as the larger of either quadratic mean of all the individual TML uncertainties of all contributing source detections or the standard deviation of all source positions, divided by the square root of the number of maps the source is detected in. arcsec DOUBLE primary pos_flag This flag indicates a potential problem with the position of this source if set to True. It is set if the uncertainties associated with the position are larger than the search radius used by the consolidation algorithm. It is also set if the maximum distance between the positions of all contributing detections is larger than the search radius used by the consolidation algorithm. The search radius is chosen as half of the FWHM of the beam profile for the respective source increased by 6” as allowance for the 3 sigma pointing uncertainty of Herschel VARCHAR primary astrom_flag Astrometry flag indicating that one or more of the contributing source detections came from a map with a positional offset greater than 5” derived from stacking at WISE 24 ?m catalog positions. A total of 140573 records was flagged in this way. VARCHAR primary nmap The number of times a source should have been detected at the list position and in the same band pass, based on the coverage maps. This value is derived by testing a 3x3 pixel square centered on the source in each coverage map. If the coverage anywhere within this square is greater than zero, the NMAP value for this object is incremented by one. INTEGER primary ndet This column contains the actual number of detections in separate maps of this object at this position and filter band. Combinations of maps into a Level 2.5 map are counted as one. There are rare cases where two close, but separate detections in the same map become part of the same object because the grouping algorithm was not able to distinguish them. In this case the source duplication flag is set. INTEGER primary dupl_flag This flag is False by default and set to True if more than one source from the same map were identified as part of this object by the object consolidation algorithm. This is a rare occurrence and mainly due to limitations of the algorithm used. The flag was set 1624 times (960,497,167 for the filter bands respectively). VARCHAR primary flux This column shows the average of the TML derived fluxes of all contributing sources, weighted with the respective TML generated uncertainties. This procedure of fitting a fixed width circular Gaussian beam profile model has proven to be superior to a number of other common methods used with SPIRE data in terms of reproducibility and photometric accuracy, down to fluxes of 30 mJy (Pearson et al. 2014). mJy DOUBLE primary fluxtml_err This column contains the propagated weighted error produced by the TML for all contributing source detections. mJy DOUBLE primary conf_err This column indicates the local confusion uncertainty in mJy. It is the average of the individual values of all contributing sources, weighted with the respective TML uncertainties. mJy DOUBLE primary flux_err This column indicates the local confusion uncertainty in mJy. It is the average of the individual values of all contributing sources, weighted with the respective TML uncertainties. mJy DOUBLE primary snr This value has been added for convenience and expresses the signal to noise ratio associated with a given object as the ratio between the Timeline Fitter flux (FLUX) and the total flux error (FLUX_ERR). DOUBLE primary insterr_flag This flag indicates that the TML returned no count for the number of readouts in the central aperture. To still be able to derive an instrument noise component, a typical number was used, based on the instrument configuration and multiplied with the number of repeats of the observation. VARCHAR primary fluxsus This column shows the average of the Sussextractor derived fluxes of all contributing sources, weighted with the respective Sussextractor generated uncertainties. mJy DOUBLE primary fluxsus_err This column contains the propagated weighted error produced by Sussextractor for all contributing source detections. mJy DOUBLE primary fluxdao This column shows the average of the Daophot derived fluxes of all contributing sources, weighted with the respective Daophot generated uncertainties. mJy DOUBLE primary fluxdao_err This column contains the propagated weighted error produced by Daophot for all contributing source detections. mJy DOUBLE primary fluxtm2 This column shows the average of the TM2 derived fluxes of all contributing sources, weighted with the respective TM2 generated uncertainties. This procedure fits an elliptical Gaussian beam profile model where the major and minor axes have been left as free fit parameters. The configuration also allows for a tilted background plane. mJy DOUBLE primary fluxtm2_err This column contains the propagated weighted error produced by TML2 for all contributing source detections. mJy DOUBLE primary fwhm1 This column contains the average FWHM of the major axes of the elliptical Gaussian beam profile models fitted during the TM2 run to all the contributing detections, weighted by their respective uncertainties. arcsec DOUBLE primary fwhm2 This column contains the average FWHM of the minor axes of the elliptical Gaussian beam profile models fitted during the TM2 run to all the contributing detections, weighted by their respective uncertainties. arcsec DOUBLE primary fwhm1_err This column contains the respective uncertainties of the weighted averages of the major and minor axes of the fitted elliptical Gaussian beam profile in arcsec. arcsec DOUBLE primary fwhm2_err This column contains the respective uncertainties of the weighted averages of the major and minor axes of the fitted elliptical Gaussian beam profile in arcsec. arcsec DOUBLE primary rot This column contains a robust average rotation angle of the elliptical Gaussian beam profile models fitted during the TM2 run to all the contributing detections. Robust meaning that all angles with uncertainties that are larger than a factor 1.5 of the median of all uncertainties of the contributing detections are removed before averaging. The rotation angle on the sky is measured from West counter-clockwise in degrees. Possible values start from 0 and are smaller than 180 deg. The average of the angles is calculated in Cartesian space to avoid problems when crossing the 180 deg threshold. Since a position angle of 180 deg is equal to 0 deg, we multiplied the position angles by 2 before averaging and divided by 2 after the back-transformation. A constant of 180 deg was added when the angle was smaller than 0 to stay within the allowed range. dec DOUBLE primary rot_err This column contains the propagated error of the rotation angle for all contributing source detections. dec DOUBLE primary pntsrc_flag The flag is set for all objects, where both the major and minor FWHM parameters are still compatible with values that are observed from point sources at a given flux level. As such it is an indicator but not conclusive, in particular not for small fluxes. VARCHAR primary extsrc_flag This flag is set if any of the major or minor FWHM is larger than the upper flux dependent threshold for point sources. VARCHAR primary lowfwhm_flag This flag is set if any of the major or minor FWHM is smaller than the lower flux dependent threshold for point sources. VARCHAR primary largegal_flag This flag is set when the catalog position is within one of the ellipses given in the 2MASS Large Galaxy Atlas (LGA) (Jarrett et al 2003) for galaxies with major axis > 1arcmin. The values are described as 'K_s (LGA/2MASS "total")' and represent the standard 2MASS aperture. If the flag is set there is a high probability that the source is part of the respective large galaxy rather than a background object. VARCHAR primary mapedge_flag The map edge flag is set when at least one of the contributing sources shows 10 or more percent of map pixels without a flux value (NaN) within the outer radius of the background annulus used by the Timeline Fitter (74”, 103”, 147”) for 250, 350, and 500 microns respectively. This condition flags catalog objects where its detection or the flux estimate may have been affected by at least one contributor being close to a map edge. 24313 objects are the edge flag set. VARCHAR primary ssocont_flag This flag is set as a warning if any of the known contributors to the catalog object is within a rectangle defined by the tracklet of a known asteroid at the time of the observation of the respective map, and the beam FWHM at the wavelength of the map. The estimated flux using a simple asteroid standard model needs to be at least at the one sigma confusion limit of Nguyen et al. (2010) of 5.8, 6.3, 6.8 mJy for 250, 350, and 500 microns respectively. 810 objects have this flag set. VARCHAR primary q3ctile As the exclusion criterion for regions with highly structured background emission is determined on the basis of the median STRN within a Q3C tile at the 22 bit level, we add the respective Q3C tile identifier to each object. It is a 19 digit number that is best interpreted using the Postgres implementation of Q3C. DOUBLE primary hsa.pacs_point_source_100 source_id The object name is an identifier consisting of two parts, acronym and sequence, and is formatted as ’HPPSCxxxA_Jhhmmss.s±ddmmss’. ’HPPSC’ stands for Herschel PACS Point Source Catalogue, xxx is the central wavelength of the band in which the source was observed, identifying the wavelength in microns, and the letter A indicates the first version of the catalogue. The second part has the format ’Jhhmmss.s+ddmmss’ derived from the source coordinates with ’J’ indicating a J2000 reference system, ’hhmmss.s’ is the Right Ascension in hours, minutes and seconds accuracy of one digits after the decimal, and ’+ddmmss’ is the Declination in signed degrees, minutes and seconds to an accuracy of one digit after the decimal. VARCHAR primary band This is one of the strings "blue","green","red" identifying the PACS detector array names for the filter bands centred at 70, 100, 160 microns, respectively. The wavelength is also specified in the name of the object. microns VARCHAR primary ra Right Ascension coordinate in a J2000.0 reference frame. This is the peak position of the SUSSEXtractor detection. The coordinates are degrees written in double precision format. deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE primary dec Declination coordinate in a J2000.0 reference frame. This is the peak position of the SUSSEXtractor detection. The coordinates are degrees written in double precision format. deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE primary raerr Positional uncertainties of each object as provided by SUSSEXtractor. Units are degrees, the data type is double precision. deg DOUBLE primary decerr Positional uncertainties of each object as provided by SUSSEXtractor. Units are degrees, the data type is double precision. deg DOUBLE primary flux This is the flux as provided by the AnnularSkyAperturePhotometry task. For objects that were identified several times across different maps, this flux corresponds to the extraction with the best average S/N, where the Ns based S/N (S/Ns)and the background RMS based S/N (S/Nr) values are taken into account. For the blue and green bands the aperture radius was 6??, for the red band 12?? (see Section 3.3 for more details). For all cases the raw flux density values were corrected for the aperture size, based on Lutz (2015). Colour corrections were not applied. The units are mJy, written as double precision. mJy DOUBLE primary snr Estimated S/N based on a statistical approach, using the S/Ns calibration surfaces. It is calculated as a function of the source flux and the Ns value. The data type is double precision. DOUBLE primary snrnoise It is calculated from the source flux and the estimated S/Ns, by dividing the flux by the S/Ns. This noise includes both the sky confusion and the instrument noise. DOUBLE primary stn Calculated as the ratio of the source flux and the RMS. Data type is double precision. DOUBLE primary rms RMS noise as measured in the blank sky apertures placed around the source. Double precision. Units are mJy. mJy DOUBLE primary strn Structure noise value obtained from the structure noise maps. Double precision, in units of MJy/sr. MJy/sr DOUBLE primary fratio The ratio of the flux density values measured in the 6th and the 1st aperture, corresponding to 4?? and 9?? in the blue and green bands, and 9?? and 14?? in the red band. DOUBLE primary fwhmxfit This column contains the FWHM values measured by the 2D Gaussian model in X and Y directions, fitted by the sourceFitter() task. If the elongated Gaussian fit was possible then both FWHMx and FWHMy are listed. If only a circular Gaussian could be fitted then FWHMy is equal to -99.9. It is written in double precision format, in units of second of arc. arcsec DOUBLE primary fwhmyfit This column contains the FWHM values measured by the 2D Gaussian model in X and Y directions, fitted by the sourceFitter() task. If the elongated Gaussian fit was possible then both FWHMx and FWHMy are listed. If only a circular Gaussian could be fitted then FWHMy is equal to -99.9. It is written in double precision format, in units of second of arc. arcsec DOUBLE primary elong_flag If an elliptical Gaussian model was fitted in the source, this column contains the ratio of the FWHMy and FWHMx. A value of 0 means that the source is circular, 0.5 means that FWHMy = 0.5 × FWHMx. If FWHMy = -99.9 (circular detection), FLAG_ELONG = 0. FLAG_ELONG is also set to 0 if the source eccentricity (FWHMx - FWHMy)/FWHMx) defined in a similar way with the FWHM values of the PACS PSF reported in Table 1, is smaller than the PSF eccentricity, Double precision format. DOUBLE primary edge_flag The position of a source with respect to the edges of the image affects the quality of the photometry, as the extraction procedure needs a large enough area to compute properly both the flux density and the background to be subtracted. Also, due to the scan speed inhomogeneities during the turnarounds, the map edges may have different noise properties than the rest of the image. BOOLEAN primary blend_flag Objects with distance within the PSF FWHM have the same value (>0) of FLAG_BLEND and they can be considered as blended sources. FLAG_BLEND = 0 means that the object is not blended with other objects. The PACS PSFs depend on the observing mode. The absolute pointing error for SPG13 (1.2??) is adopted as uncertainty. DOUBLE primary warmat Flag indicating that the observation was affected by "warm" attitude. The term refers to spacecraft attitudes in which the star-tracker support structure is subject to thermal distortions as was not completely shaded from sunlight. This has an impact on the pointing accuracy. Data type is Boolean. BOOLEAN primary obsid The term is the observation identifier for the Herschel observations . It is a 10 digit integer, starting always with 1342. The column lists the first OBSID from the list that built the L2.5/L3 map. It corresponds to the meta keyword obsid001. meta.ref.url Acess.reference VARCHAR primary ssomap_flag Maps of solar system objects have typically been observed in tracking mode, but were reprocessed in the ’rest’ sky frame for the HPPSC, and may be contaminated by the moving targets. The affected OBSIDs are marked with an ’ssomap’ flag. BOOLEAN primary hsa.v_proposal_observation band VARCHAR duration DOUBLE instrument_group VARCHAR instrument_oid INTEGER observation_id VARCHAR observation_oid INTEGER observing_mode_oid INTEGER proposal_id VARCHAR proposal_key VARCHAR subinstrument VARCHAR hsa.hifi_spectral_line_native obsid Observation ID meta.ref.url Acess.reference VARCHAR primary source_id Name of the source VARCHAR primary ra Right Ascension coordinate deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE primary dec Declination coordinate deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE primary observing_mode HIFI Observing mode name VARCHAR primary spectrograph Name of spectrometer backend. Save for a handful of exceptions, it will always be "WBS-HV" as both polarisations should have been averaged to form the input spectrum VARCHAR primary spectra_resolution Spectral resolution of input spectrum. For the default LineCatalogue, this corresponds to the native resolution (around 1 MHz), while for smoothed tables, it indicates the resulting spectral bin size after smoothing MHz DOUBLE primary database Data-base from which the line spectroscopy parameters are taken (JPLor CDMS) VARCHAR primary species Name of the molecular or atomic species VARCHAR primary transition Name of transition VARCHAR primary rest_frequency Frequency of the line transition in the LSR GHz DOUBLE primary eup Upper energy level Eup of the line K DOUBLE primary aij Einstein coefficient Aij 1/s DOUBLE primary position Fitted position of the line centroid GHz DOUBLE primary std_position Standard deviation error on the above fitted position GHz DOUBLE primary side_band VARCHAR primary v0 Position of the velocity centroid km/s DOUBLE primary std_v0 Standard deviation error on the fitted centroid km/s DOUBLE primary width Line width of the Gaussian line fit. Not provided in case of smoothed tables km/s DOUBLE primary std_width Standard deviation error on the fitted line width km/s DOUBLE primary flux Integrated intensity of the fitted line. Note that this number is negative in case of absorption lines because the spectra used to perform the fit have been baseline-subtracted. Not provided in case of smoothed tables K.km/s DOUBLE primary std_flux Standard deviation error on the integrated intensity K.km/s DOUBLE primary background Continuum level estimated within the frequency interval used for the fit. Because the input spectra have had their baseline subtracted, this level is essentially zero K DOUBLE primary std_background Standard deviation error on the above continuum level K DOUBLE primary rms RMS noise level of the spectra estimated from the spectrum on two windows of 50 MHz on either side of the line profile K DOUBLE primary signal_to_noise_ratio Fitted line peak signal-to-noise ratio DOUBLE primary evidence Provides a quality measure of the Gaussian fit (based on a Bayesianstatistics fitter) DOUBLE primary peak_position Frequency position of the fitted line peak GHz DOUBLE primary lower_frequency_fit_window Lower frequency of the interval used to perform the Gaussian fit GHz DOUBLE primary upper_frequency_fit_window Higher frequency of the interval used to perform the Gaussian fit GHz DOUBLE primary hsa.pacs_point_source_160 source_id The object name is an identifier consisting of two parts, acronym and sequence, and is formatted as ’HPPSCxxxA_Jhhmmss.s±ddmmss’. ’HPPSC’ stands for Herschel PACS Point Source Catalogue, xxx is the central wavelength of the band in which the source was observed, identifying the wavelength in microns, and the letter A indicates the first version of the catalogue. The second part has the format ’Jhhmmss.s+ddmmss’ derived from the source coordinates with ’J’ indicating a J2000 reference system, ’hhmmss.s’ is the Right Ascension in hours, minutes and seconds accuracy of one digits after the decimal, and ’+ddmmss’ is the Declination in signed degrees, minutes and seconds to an accuracy of one digit after the decimal. VARCHAR primary band This is one of the strings "blue","green","red" identifying the PACS detector array names for the filter bands centred at 70, 100, 160 microns, respectively. The wavelength is also specified in the name of the object. microns VARCHAR primary ra Right Ascension coordinate in a J2000.0 reference frame. This is the peak position of the SUSSEXtractor detection. The coordinates are degrees written in double precision format. deg pos.eq.ra;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C1 DOUBLE primary dec Declination coordinate in a J2000.0 reference frame. This is the peak position of the SUSSEXtractor detection. The coordinates are degrees written in double precision format. deg pos.eq.dec;meta.main Char.SpatialAxis.Coverage.Location.Coord.Position2D.Value2.C2 DOUBLE primary raerr Positional uncertainties of each object as provided by SUSSEXtractor. Units are degrees, the data type is double precision. deg DOUBLE primary decerr Positional uncertainties of each object as provided by SUSSEXtractor. Units are degrees, the data type is double precision. deg DOUBLE primary flux This is the flux as provided by the AnnularSkyAperturePhotometry task. For objects that were identified several times across different maps, this flux corresponds to the extraction with the best average S/N, where the Ns based S/N (S/Ns)and the background RMS based S/N (S/Nr) values are taken into account. For the blue and green bands the aperture radius was 6??, for the red band 12?? (see Section 3.3 for more details). For all cases the raw flux density values were corrected for the aperture size, based on Lutz (2015). Colour corrections were not applied. The units are mJy, written as double precision. mJy DOUBLE primary snr Estimated S/N based on a statistical approach, using the S/Ns calibration surfaces. It is calculated as a function of the source flux and the Ns value. The data type is double precision. DOUBLE primary snrnoise It is calculated from the source flux and the estimated S/Ns, by dividing the flux by the S/Ns. This noise includes both the sky confusion and the instrument noise. DOUBLE primary stn Calculated as the ratio of the source flux and the RMS. Data type is double precision. DOUBLE primary rms RMS noise as measured in the blank sky apertures placed around the source. Double precision. Units are mJy. mJy DOUBLE primary strn Structure noise value obtained from the structure noise maps. Double precision, in units of MJy/sr. MJy/sr DOUBLE primary fratio The ratio of the flux density values measured in the 6th and the 1st aperture, corresponding to 4?? and 9?? in the blue and green bands, and 9?? and 14?? in the red band. DOUBLE primary fwhmxfit This column contains the FWHM values measured by the 2D Gaussian model in X and Y directions, fitted by the sourceFitter() task. If the elongated Gaussian fit was possible then both FWHMx and FWHMy are listed. If only a circular Gaussian could be fitted then FWHMy is equal to -99.9. It is written in double precision format, in units of second of arc. arcsec DOUBLE primary fwhmyfit This column contains the FWHM values measured by the 2D Gaussian model in X and Y directions, fitted by the sourceFitter() task. If the elongated Gaussian fit was possible then both FWHMx and FWHMy are listed. If only a circular Gaussian could be fitted then FWHMy is equal to -99.9. It is written in double precision format, in units of second of arc. arcsec DOUBLE primary elong_flag If an elliptical Gaussian model was fitted in the source, this column contains the ratio of the FWHMy and FWHMx. A value of 0 means that the source is circular, 0.5 means that FWHMy = 0.5 × FWHMx. If FWHMy = -99.9 (circular detection), FLAG_ELONG = 0. FLAG_ELONG is also set to 0 if the source eccentricity (FWHMx - FWHMy)/FWHMx) defined in a similar way with the FWHM values of the PACS PSF reported in Table 1, is smaller than the PSF eccentricity, Double precision format. DOUBLE primary edge_flag The position of a source with respect to the edges of the image affects the quality of the photometry, as the extraction procedure needs a large enough area to compute properly both the flux density and the background to be subtracted. Also, due to the scan speed inhomogeneities during the turnarounds, the map edges may have different noise properties than the rest of the image. BOOLEAN primary blend_flag Objects with distance within the PSF FWHM have the same value (>0) of FLAG_BLEND and they can be considered as blended sources. FLAG_BLEND = 0 means that the object is not blended with other objects. The PACS PSFs depend on the observing mode. The absolute pointing error for SPG13 (1.2??) is adopted as uncertainty. DOUBLE primary warmat Flag indicating that the observation was affected by "warm" attitude. The term refers to spacecraft attitudes in which the star-tracker support structure is subject to thermal distortions as was not completely shaded from sunlight. This has an impact on the pointing accuracy. Data type is Boolean. BOOLEAN primary obsid The term is the observation identifier for the Herschel observations . It is a 10 digit integer, starting always with 1342. The column lists the first OBSID from the list that built the L2.5/L3 map. It corresponds to the meta keyword obsid001. meta.ref.url Acess.reference VARCHAR primary ssomap_flag Maps of solar system objects have typically been observed in tracking mode, but were reprocessed in the ’rest’ sky frame for the HPPSC, and may be contaminated by the moving targets. The affected OBSIDs are marked with an ’ssomap’ flag. BOOLEAN primary hsa.ancillary ancillary_oid INTEGER data_repository VARCHAR filename VARCHAR file_size BIGINT release_note VARCHAR title VARCHAR hsa.metadata_expert_panels band HIFI Local Oscillator sub-band: 1a, 1b, 2a, 2b, ..., 7a, 7b VARCHAR biasmode The SPIRE bias mode defines whether the detector dynamic range was optimised for nominal (<500 Jy) or bright (>500 Jy) sources. VARCHAR blue PACS blue filter selection: blue1 or blue2 VARCHAR chopnod The telescope background measurement is obtained via rapid on-off chopping while the grating scan pattern is executed (ChopNod), or from in a unique OFF position where the same grating scan pattern is repeated (Unchopped). BOOLEAN chopper_throw The angular separation for the telescope background measurement in ChopNod mode can be Small (1.5 arcminutes), Medium (3 arc minutes), or Large (6 arcminutes). VARCHAR clbpdtct Indicates a SPIRE cooler burp BOOLEAN cmdres SPIRE Spec commanded resolution which depends on the actual distance that the scanning mirror moved - it is distinct from the processed resolution because some modes are simplified for the pipeline (CR treated as HR, and MR treated as LR). High resolution and calibration resolution are 1.184 GHz; Medium resolution is 7.2 GHz; Low resolution is 26.8 GHz. VARCHAR dither PACS dither pattern. Only relevant for the Point Source Mode. BOOLEAN drftnsct HIFI drift noise contribution DOUBLE faintlin PACS Spec faint line mode selected BOOLEAN freqmax HIFI observed max frequency in freqFrame (SPECSYS) DOUBLE freqmin HIFI observed min frequency in freqFrame (SPECSYS) DOUBLE freq_thr HIFI frequency change of the local oscillator in the reference phase of Frequency Switch observations. The magnitude depends on observing band; a small throw is about 96MHz, a large throw is about 300 MHz or 190 MHz (bands 6&7). VARCHAR instrument_mode The observing scheme of the PACS Spectrometer is defined for individual spectral lines (Line Spectroscopy), or for specified spectral ranges and the Spectral Energy Distribution mode (Range Spectroscopy). VARCHAR instrument_oid Database index number INTEGER is_hrsh HIFI science data are obtained with HRS-H BOOLEAN is_hrsv HIFI science data are obtained with HRS-V BOOLEAN is_wbsh HIFI science data are obtained with WBS-H BOOLEAN is_wbsv HIFI science data are obtained with WBS-V BOOLEAN lfreqmax HIFI observed max frequency for LSB in freqFrame (SPECSYS) DOUBLE lfreqmin HIFI observed min frequency for LSB in freqFrame (SPECSYS) DOUBLE line1 PACS spectral line/range: wavelength, reps, id VARCHAR line10 PACS spectral line/range: wavelength, reps, id VARCHAR line2 PACS spectral line/range: wavelength, reps, id VARCHAR line3 PACS spectral line/range: wavelength, reps, id VARCHAR line4 PACS spectral line/range: wavelength, reps, id VARCHAR line5 PACS spectral line/range: wavelength, reps, id VARCHAR line6 PACS spectral line/range: wavelength, reps, id VARCHAR line7 PACS spectral line/range: wavelength, reps, id VARCHAR line8 PACS spectral line/range: wavelength, reps, id VARCHAR line9 PACS spectral line/range: wavelength, reps, id VARCHAR lodoppav HIFI average LO frecuency Doppler-corrected to freqFrame (SPECSYS) DOUBLE lofreq HIFI actual local oscillator frequency DOUBLE lofrqend HIFI actual end local oscillator frequency DOUBLE lofrqmax HIFI max LO frecuency of the spectral scan Doppler-corrected to freqFrame (SPECSYS) DOUBLE lofrqmin HIFI min LO frecuency of the spectral scan Doppler-corrected to freqFrame (SPECSYS) DOUBLE lofrqsta HIFI actual start local oscillator frequency DOUBLE maphgt SPIRE height of the map in arcmin. Min value = 4 and max = 930 DOUBLE maplen SPIRE length of the map in arcmin. Min value = 4 and max = 232.5 DOUBLE mapsampl SPIRE spatial sampling of map VARCHAR mapscanrate PACS scan speed for Parallel mode VARCHAR mapscanspeed PACS scan map speed for PACS photometry VARCHAR metadata_expert_panels_oid Database index number INTEGER noismaxd HIFI noise DSB at maximum bandwith H and V polarization averaged DOUBLE noismaxl HIFI noise LSB at maximum bandwith H and V polarization averaged DOUBLE noismaxs HIFI deconvolved SSB noise at maximum bandwith H and V polarization averaged DOUBLE noismaxu HIFI noise USB at maximum bandwith H and V polarization averaged DOUBLE noismind HIFI noise DSB at minimum bandwith H and V polarization averaged DOUBLE noisminl HIFI noise LSB at minimum bandwith H and V polarization averaged DOUBLE noismins HIFI deconvolved SSB noise at minimum bandwith H and V polarization averaged DOUBLE noisminu HIFI noise USB at minimum bandwith H and V polarization averaged DOUBLE nrastcol PACS Spec number of raster columns INTEGER nraster The number of SPIRE raster points, determined by the map size. For a single pointing observation the value is 1. BIGINT nrastlin PACS Spec number of raster lines INTEGER nsmaxwid HIFI maximum bandwidth for noise predictions MHz DOUBLE nsminwid HIFI minimum bandwidth for noise predictions MHz DOUBLE nsreffrq HIFI noise reference frequency GHz DOUBLE numrep The number of SPIRE scan pair (forward+reverse) repeats. INTEGER observation_oid Database index number INTEGER observing_mode_oid Database index number INTEGER observing_mode_settings Observing mode settings VARCHAR obs_mode Observation mode VARCHAR ordersel PACS blue band (order 2: 50-70 microns; order 3: 70-100 microns) VARCHAR pacs_phot_gain PACS phot gain settings (high or low) VARCHAR point_mode HIFI Pointing mode VARCHAR posangle The position angle of the telescope pointing DOUBLE prcasres For SPIRE Spec the final spectral resolution of the processed data can be either High (1.184 GHz) or Low (26.8 GHz), or contain both (H+L). VARCHAR processing_params Allthe PACS observations involved in the production of level2.5/level3 products text rasstepc PACS Spec raster point step DOUBLE rasstepl PACS Spec raster line step DOUBLE redshft Redshif type: redshift or optical text redshftv Redshift value DOUBLE reduncy HIFI Spectral Scan redundancy requested INTEGER rmsmaxd HIFI rms noise DSB at maximum bandwith H and V polarization averaged DOUBLE rmsmaxl HIFI rms noise LSB at maximum bandwith H and V polarization averaged DOUBLE rmsmaxs HIFI rms deconvolved SSB noise at maximum bandwith H and V polarization averaged DOUBLE rmsmaxu HIFI rms noise USB at maximum bandwith H and V polarization averaged DOUBLE rmsmind HIFI rms noise DSB at minimum bandwith H and V polarization averaged DOUBLE rmsminl HIFI rms noise LSB at minimum bandwith H and V polarization averaged DOUBLE rmsmins HIFI rms deconvolved SSB noise at minimum bandwith H and V polarization averaged DOUBLE rmsminu HIFI rms noise USB at minimum bandwith H and V polarization averaged DOUBLE rmsnatd HIFI rms deconvolved DSB noise rescaled to native WBS resolution H and V polarization averaged DOUBLE rmsnatl HIFI rms deconvolved LSB noise rescaled to native WBS resolution H and V polarization averaged DOUBLE rmsnats HIFI rms deconvolved SSB noise rescaled to native WBS resolution H and V polarization averaged DOUBLE rmsnatu HIFI rms deconvolved USB noise rescaled to native WBS resolution H and V polarization averaged DOUBLE rnghi01 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi02 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi03 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi04 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi05 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi06 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi07 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi08 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi09 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi10 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi11 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi12 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi13 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi14 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi15 PACS Range Spec high wavelength end of range scanned DOUBLE rnghi16 PACS Range Spec high wavelength end of range scanned DOUBLE rnglo01 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo02 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo03 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo04 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo05 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo06 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo07 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo08 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo09 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo10 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo11 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo12 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo13 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo14 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo15 PACS Range Spec lower wavelength end of range scanned DOUBLE rnglo16 PACS Range Spec lower wavelength end of range scanned DOUBLE saamean Avergade Solar Aspect Angle DOUBLE saarms Standard deviation of the Solar Aspect Angle DOUBLE scandir SPIRE Phot scan direction. For normal cross scanned large maps select Scan Angles A and B. For parallel maps choose either A or B where A=42.4 degrees, B=-42.4 degrees to the SPIRE arrays short axis (Z). VARCHAR scanspd The scanning speed of the telescope in arcsec/s. For SPIRE large maps the Nominal speed was 30"/s and the fast speed was 60"/s. For parallel mode the fast speed was 60"/s and the slow speed was 20"/s. VARCHAR scanvelo PACS nominal scanning velocity arcsec/s DOUBLE source PACS Phot pointing mode: point: single, large: mapping VARCHAR tmbreffq For HIFI the temperature (main beam) at noise reference frequency DOUBLE totnseff For HIFI total noise efficiency DOUBLE ufreqmax Observed (sky) max frequency for USB DOUBLE ufreqmin Observed (sky) min frequency for USB DOUBLE veldef The velocity definition and frame VARCHAR vframe The velocity definition and frame for HIFI DOUBLE wavedens The spectral sampling for PACS Range Spectroscopy can be High (a resolution element is seen at least 3 times in every detector) or Nyquist (a resolution element is seen at least 3 times between all 16 detectors) VARCHAR pubtool pubtool.institutions affiliation VARCHAR city VARCHAR country VARCHAR direction VARCHAR geolocating_method VARCHAR institution_oid INTEGER latitude DOUBLE longitude DOUBLE name VARCHAR pubtool.v_first_pub_date bib_code VARCHAR instrument_name VARCHAR observation_id VARCHAR proposal_key VARCHAR pubdate TIMESTAMP pubtool.v_first_pub_date_single bib_code VARCHAR instrument_name VARCHAR observation_id VARCHAR proposal_key VARCHAR pubdate TIMESTAMP pubtool.archival_type archival_type_oid INTEGER description VARCHAR pubtool.publication abstract VARCHAR archival_type INTEGER authors VARCHAR authors_plain VARCHAR bib_code VARCHAR end_page VARCHAR eprint VARCHAR journal VARCHAR journal_group VARCHAR keywords VARCHAR num_citations INTEGER num_observations INTEGER objects VARCHAR pubdate TIMESTAMP start_page VARCHAR status VARCHAR title VARCHAR volume VARCHAR pubtool.publication_details ads_link VARCHAR bib_code VARCHAR comments VARCHAR doi VARCHAR hipe_version VARCHAR user_catalog_data BOOLEAN user_image_data BOOLEAN user_spectra_data BOOLEAN vizier_catalog_id VARCHAR vizier_catalog_name VARCHAR pubtool.authors_institutions author_oid INTEGER bib_code VARCHAR institution_oid INTEGER pubtool.publication_observation bib_code VARCHAR calibration BOOLEAN duration DOUBLE failed BOOLEAN instrument_group VARCHAR instrument_name VARCHAR observation_id VARCHAR proposal_author VARCHAR proposal_id VARCHAR proposal_key VARCHAR standard BOOLEAN subinstrument VARCHAR pubtool.authors author_oid INTEGER bib_code VARCHAR first_author BOOLEAN name VARCHAR name_plain VARCHAR updp2 updp2.latest_observation_updp file_oid INTEGER instrument_oid INTEGER observation_id VARCHAR request_oid INTEGER updp2.vizier_links updp2.latest_unique_observation_requests instrument_oid INTEGER max_request_oid INTEGER num_requests BIGINT observation_id VARCHAR updp2.files filename VARCHAR file_oid INTEGER file_size BIGINT file_type_oid INTEGER main_postcard BOOLEAN request_oid INTEGER vizier_link VARCHAR updp2.latest_requests abstract text author text category VARCHAR date_active_version TIMESTAMP date_ingest_completed TIMESTAMP date_ingest_requested TIMESTAMP date_ingest_started TIMESTAMP directory VARCHAR full_retrieval_file_size BIGINT full_retrieval_path VARCHAR is_active_version BOOLEAN job_id VARCHAR keyword VARCHAR rel_notes_file VARCHAR request_file VARCHAR request_oid INTEGER title text version_change_log VARCHAR version_number INTEGER updp2.unique_observation_updp aor VARCHAR category VARCHAR dec DOUBLE duration DOUBLE end_time TIMESTAMP fov VARCHAR instrument_oid INTEGER is_public BOOLEAN keyword VARCHAR naif_id VARCHAR num_requests BIGINT observation_id VARCHAR observation_oid INTEGER observer VARCHAR observing_mode_oid INTEGER obsstate VARCHAR od_number BIGINT polygon_fov VARCHAR prop_end TIMESTAMP proposal_id VARCHAR ra DOUBLE request_oid INTEGER spg_id VARCHAR start_time TIMESTAMP status VARCHAR target_name VARCHAR urn_version INTEGER