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J/ApJ/704/842       VIRUS-P spectroscopy of NGC 5194             (Blanc+, 2009)

The spatially resolved star formation law from integral field spectroscopy: VIRUS-P observations of NGC 5194. Blanc G.A., Heiderman A., Gebhardt K., Evans N.J., Adams J. <Astrophys. J., 704, 842-862 (2009)> =2009ApJ...704..842B
ADC_Keywords: Galaxies, spectra ; Interstellar medium ; Spectroscopy Keywords: galaxies: formation - galaxies: individual (NGC 5194) - galaxies: ISM - galaxies: spiral - ISM: structure - stars: formation Abstract: We investigate the relation between the star formation rate (SFR) surface density (ΣSFR) and the mass surface density of gas (Σgas) in NGC 5194 (a.k.a. M51a, Whirlpool Galaxy). Visible Integral field Replicable Unit Spectrograph Prototype (VIRUS-P) integral field spectroscopy of the central 4.1x4.1kpc2 of the galaxy is used to measure Hα, Hβ, [OIII]5007, [NII]6548,6584, and [SII]6717,6731 emission line fluxes for 735 regions ∼170pc in diameter. We use the Balmer decrement to calculate nebular dust extinctions, and correct the observed fluxes in order to accurately measure ΣSFR in each region. Archival HI 21cm and CO maps with spatial resolution similar to that of VIRUS-P are used to measure the atomic and molecular gas surface density for each region. Description: We obtained spatially resolved spectroscopy over the central 4.1x4.1kpc2 region of NGC 5194 on the night of 2008 April 4, using VIRUS-P on the 2.7m Harlan J. Smith telescope at McDonald Observatory. The spectrograph was used in a red setup under which it samples a wavelength range of 4570-6820Å with a spectral resolution of ∼5.0Å (FWHM). Emission line fluxes of all lines for all fibers are given in Table 1. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 141 735 Nebular emission line fluxes, gas surface densities, and SFR surface densities
See also: J/ApJ/671/333 : Aperture photometry in NGC 5194 (Kennicutt+, 2007) J/ApJ/633/871 : Positions and photometry of HII knots in M51 (Calzetti+, 2005) J/A+A/309/446 : HII Regions in M51 (Petit+, 1996) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- ID Running identification number 5- 6 I2 h RAh Hour of Right Ascension (J2000) 8- 9 I2 min RAm Minute of Right Ascension (J2000) 11- 15 F5.2 s RAs Second of Right Ascension (J2000) 17 A1 --- DE- Sign of the Declination (J2000) 18- 19 I2 deg DEd Degree of Declination (J2000) 21- 22 I2 arcmin DEm Arcminute of Declination (J2000) 24- 27 F4.1 arcsec DEs Arcsecond of Declination (J2000) 29- 34 F6.2 10-19W/m2 Hb The Hβ line flux (1) 36- 39 F4.2 10-19W/m2 e_Hb Uncertainty in Hb (1) 41- 46 F6.2 10-19W/m2 N6548 The [NII](6548) line flux (1) 48- 51 F4.2 10-19W/m2 e_N6548 Uncertainty in N6548 (1) 53- 58 F6.2 10-19W/m2 Ha The Hα line flux (1) 60- 63 F4.2 10-19W/m2 e_Ha Uncertainty in Ha (1) 65- 71 F7.2 10-19W/m2 N6584 The [NII](6584) line flux (1) 73- 76 F4.2 10-19W/m2 e_N6584 Uncertainty in N6584 (1) 78- 83 F6.2 10-19W/m2 S6717 The [SII](6717) line flux (1) 85- 88 F4.2 10-19W/m2 e_S6717 Uncertainty in S6717 (1) 90- 95 F6.2 10-19W/m2 S6731 The [SII](6731) line flux (1) 97-100 F4.2 10-19W/m2 e_S6731 Uncertainty in S6731 (1) 102-108 F7.2 Msun/pc2 SigH2 Molecular H2 gas surface density 110-114 F5.2 Msun/pc2 e_SigH2 Uncertainty in SigH2 116-120 F5.2 Msun/pc2 SigHI Atomic HI gas surface density 122-125 F4.2 Msun/pc2 e_SigHI Uncertainty in SigHI 127-133 F7.5 Msun/yr/kpc2 SigSFR Star formation rate surface density 135-141 F7.5 Msun/yr/kpc2 e_SigSFR Uncertainty in SigSFR
Note (1): In units of 10-16erg/s/cm2.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 21-Nov-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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