Data model: galSpecExtra

General description: Physical parameter measurements for fibers for which the MPA-JHU spectroscopic parameters pipeline has been run. This file is built out of a similar one in the galspec SVN product. It is designed to be line-by-line matched with the specObj list of all spectra. There is further information about the MPA-JHU results in the parallel files galSpecInfo, galSpecLine, and galSpecIndx. ID values in galSpecInfo are set to -1 for cases where there were no results from the MPA-JHU pipeline. In some cases, the pipeline was run but we don't believe the results are reliable, in which case the column "RELIABLE" in galSpecInfo is set to zero.

Naming convention: galSpecExtra-[DRNAME].fits

Approximate size: 400 Mbytes.

File type: FITS

Read by products: sas

Written by products: sas

Required column names:

• specObjID (int64): Unique ID
• bptclass (int16): Emission line classification based on the BPT diagram using the methodology described in Brinchmann et al (2004). -1 means unclassifiable, 1 is star-forming, 2 means low S/N star-forming, 3 is composite, 4 AGN (excluding liners) and 5 is a low S/N LINER.
• oh_p2p5 (float32): The 2.5 percentile of the Oxygen abundance derived using Charlot & Longhetti models. The values are reported as 12 + Log O/H. See Tremonti et al (2004) and Brinchmann et al (2004) for details.
• oh_p16 (float32): The 16 percentile of the Oxygen abundance derived using Charlot & Longhetti models. The values are reported as 12 + Log O/H. See Tremonti et al (2004) and Brinchmann et al (2004) for details.
• oh_p50 (float32): The median estimate of the Oxygen abundance derived using Charlot & Longhetti models. The values are reported as 12 + Log O/H. See Tremonti et al (2004) and Brinchmann et al (2004) for details.
• oh_p84 (float32): The 84th percentile of the Oxygen abundance derived using Charlot & Longhetti models. The values are reported as 12 + Log O/H. See Tremonti et al (2004) and Brinchmann et al (2004) for details.
• oh_p97p5 (float32): The 97.5 percentile of the Oxygen abundance derived using Charlot & Longhetti models. The values are reported as 12 + Log O/H. See Tremonti et al (2004) and Brinchmann et al (2004) for details.
• oh_entropy (float32): The entropy (Sum p*lg(p)) of the PDF of 12 + Log O/H
• lgm_tot_p2p5 (float32): The 2.5 percentile of the Log total stellar mass PDF using model photometry. (Log)
• lgm_tot_p16 (float32): The 16th percentile of the Log total stellar mass PDF using model photometry. (Log)
• lgm_tot_p50 (float32): The median estimate of the Log total stellar mass PDF using model photometry. (Log)
• lgm_tot_p84 (float32): The 84th percentile of the Log total stellar mass PDF using model photometry. (Log)
• lgm_tot_p97p5 (float32): The 97.5 percentile of the Log total stellar mass PDF using model photometry. (Log)
• lgm_fib_p2p5 (float32): The 2.5 percentile of the Log stellar mass within the fibre PDF using fibre photometry. (Log)
• lgm_fib_p16 (float32): The 16th percentile of the Log stellar mass within the fibre PDF using fibre photometry. (Log)
• lgm_fib_p50 (float32): The median estimate of the Log stellar mass within the fibre PDF using fibre photometry. (Log)
• lgm_fib_p84 (float32): The 84th percentile of the Log stellar mass within the fibre PDF using fibre photometry. (Log)
• lgm_fib_p97p5 (float32): The 97.5 percentile of the Log stellar mass within the fibre PDF using fibre photometry. (Log)
• sfr_tot_p2p5 (float32): The 2.5 percentile of the Log total SFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• sfr_tot_p16 (float32): The 16th percentile of the Log total SFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• sfr_tot_p50 (float32): The median estimate of the Log total SFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• sfr_tot_p84 (float32): The 84th percentile of the Log total SFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• sfr_tot_p97p5 (float32): The 97.5 percentile of the Log total SFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• sfr_tot_entropy (float32): The entropy (Sum p*lg(p)) of the PDF of the total SFR
• sfr_fib_p2p5 (float32): The 2.5 percentile of the Log SFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• sfr_fib_p16 (float32): The 16th percentile of the Log SFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• sfr_fib_p50 (float32): The median estimate of the Log SFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• sfr_fib_p84 (float32): The 84th percentile of the Log SFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• sfr_fib_p97p5 (float32): The 97.5 percentile of the Log SFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• sfr_fib_entropy (float32): The entropy (Sum p*lg(p)) of the PDF of the fiber SFR
• specsfr_tot_p2p5 (float32): The 2.5 percentile of the Log total SPECSFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• specsfr_tot_p16 (float32): The 16th percentile of the Log total SPECSFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• specsfr_tot_p50 (float32): The median estimate of the Log total SPECSFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• specsfr_tot_p84 (float32): The 84th percentile of the Log total SPECSFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• specsfr_tot_p97p5 (float32): The 97.5 percentile of the Log total SPECSFR PDF. This is derived by combining emission line measurements from within the fibre where possible and aperture corrections are done by fitting models ala Gallazzi et al (2005), Salim et al (2007) to the photometry outside the fibre. For those objects where the emission lines within the fibre do not provide an estimate of the SFR, model fits were made to the integrated photometry. (Log)
• specsfr_tot_entropy (float32): The entropy (Sum p*lg(p)) of the PDF of the total SPECSFR
• specsfr_fib_p2p5 (float32): The 2.5 percentile of the Log SPECSFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• specsfr_fib_p16 (float32): The 16th percentile of the Log SPECSFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• specsfr_fib_p50 (float32): The median estimate of the Log SPECSFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• specsfr_fib_p84 (float32): The 84th percentile of the Log SPECSFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• specsfr_fib_p97p5 (float32): The 97.5 percentile of the Log SPECSFR within the fiber PDF. For galaxies of the star-forming class, emission lines were used (c.f. Brinchmann et al 2004) while for others models were fit to the fibre photometry.. (Log)
• specsfr_fib_entropy (float32): The entropy (Sum p*lg(p)) of the PDF of the fiber SPECSFR