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J/A+A/429/559       Diffuse Interstellar Bands in NGC 1448    (Sollerman+, 2005)

Diffuse Interstellar Bands in NGC 1448. Sollerman J., Cox N., Mattila S., Ehrenfreund P., Kaper L., Leibundgut B., Lundqvist P. <Astron. Astrophys. 429, 559 (2005)> =2005A&A...429..559S
ADC_Keywords: Supernovae ; Spectroscopy ; Interstellar medium Keywords: supernovae: individual: SN 2001el, SN 2003hn - galaxies: individual: NGC 1448 - ISM: lines and bands - supernovae: general Abstract: We present spectroscopic VLT/UVES observations of two emerging supernovae, the Type Ia SM 2001el and the Type II SN 2003hn, in the spiral galaxy NGC 1448. Our high resolution and high signal-to-noise spectra display atomic lines of Ca II, Na I, Ti II and K I in the host galaxy. In the line of sight towards SN 2001el, we also detect over a dozen diffuse interstellar bands (DIBs) within NGC 1448. Description: table3 lists the VPFIT parameters (velocity v, Doppler parameter b and column density N) for the components of the observed atomic interstellar lines of Ca II, Ti II, Na I and K I towards SN 2001el and SN 2003hn. In the last column we give the total column density, summed over the individual components. Objects: ----------------------------------------- RA (2000) DE Designation(s) ----------------------------------------- 03 44 30.6 -44 38 23 SN 2001el 03 44 36.1 -44 37 49 SN 2003hn ----------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 74 44 VPFIT parameters fig2.ps 93 2191 *Interstellar atomic Milky Way components of Ca II K in the line-of-sight towards SN 2001el and SN 2003hn fig4.ps 93 9502 *λ6284 DIB and λ6270 DIB spectra
Note on fig2.ps: The black dashed lines refer to the fits by VPFIT, and the grey dots to the observed UVES spectra. For velocities, column densities and Doppler parameters of the fits we refer to table3.dat. The numbered symbols (+) at the top indicate the positions of the fitted velocity components. The lower spectrum has been displaced vertically for clarity. A high velocity cloud at ∼160km/s can also be seen towards SN 2001el (component 4). Note on fig4.ps: The λ6284 DIB towards SN 2001el is redshifted to 6308Å and is clearly separated from the narrow telluric O2 complex at ∼6278Å (bottom). Note also the λ6270 DIB at 6294Å. For illustrative purposes we show both the telluric uncorrected and corrected λ,6284 DIB for SN 2001el (bottom and middle). These spectra have been displaced vertically for clarity. For SN 2003hn only the telluric corrected spectrum is shown (top). In this sight line we detect the λ6284 DIB at λ6312.
See also: II/135 : Suppl. to Diffuse Interstellar Band Measurements (Guarinos, 1988) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Gal Galaxy (MW for Milky Way or NGC 1448) (1) 11- 18 A8 --- SN SN designation 20- 23 A4 --- Ion Ion designation (2) 25 I1 --- Comp Component number 28- 34 F7.2 km/s Vel Velocity 36- 39 F4.1 km/s e_Vel rms uncertainty on Vel 41- 44 F4.1 km/s b ? Doppler parameter (3) 46- 48 F3.1 km/s e_b ? rms uncertainty on b 50- 54 F5.2 [cm-2] logN Column density 56- 59 F4.2 [cm-2] e_logN rms uncertainty on logN 61- 65 F5.2 [cm-2] logNtot Total column density of the ion summed over the individual components 67- 70 F4.2 [cm-2] e_logNtot rms uncertainty on logNTot 72- 74 A3 --- n_logNtot Number of the components used for the total column density, when not all (only for SN2001el CaII)
Note (1): The interstellar atomic absorption lines detected are from the Milky Way (MW) or from NGC 1448. Note (2): We use the doublet lines of CaII, NaI and KI to constrain the least square fitting routine employed by VPFIT Note (3): The Doppler parameter, b, has for each atomic line been set equal for all components.
Acknowledgements: Jesper Sollerman, jesper(at)astro.su.se
(End) Patricia Vannier [CDS] 16-Sep-2004
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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