J/A+A/618/A3 NGC 300 MUSE spectroscopy for central fields (Roth+, 2018)
MUSE crowded field 3D spectroscopy in NGC 300.
I. First results from central fields.
Roth, M.M., Sandin, C., Kamann, S., Husser T.-O., Weilbacher P.M.,
Monreal-Ibero A., Bacon R., den Brok M., Dreizler S., Kelz A.,
Marino R.A., Steinmetz M.
<Astron. Astrophys. 618, A3 (2018)>
=2018A&A...618A...3R 2018A&A...618A...3R (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Galaxies, spectra; Spectrophotometry
Keywords: galaxies: stellar content - stars: AGB and post-AGB -
stars: Wolf-Rayet - ISM: supernova remnants - HII regions -
planetary nebulae: general
Abstract:
As a new approach to the study of resolved stellar populations in
nearby galaxies, we present a pilot study in NGC300 to demonstrate
that integral field spectroscopy with high spatial resolution and
excellent seeing conditions reaches an unprecedented depth in severely
crowded fields.
Observations by MUSE with seven pointings in NGC 300 have resulted in
data cubes that are analyzed in four ways: (1) Point spread
function-fitting 3D spectroscopy with PampelMUSE, as already
successfully pioneered in globular clusters, yields de-blended spectra
of individually distinguishable stars, thus providing a complete
inventory of blue and red supergiants, and asymptotic giant branch
(AGB) stars of type M and C. The technique is also applicable to
emission line point sources and provides samples of planetary nebulae
(PNe) that are complete down to m5007=28. (2) Pseudo-monochromatic
images, created at the wavelengths of the most important emission
lines and corrected for continuum light with the P3D visualization
tool, provide maps of HII regions, supernova remnants (SNR), and
the diffuse interstellar medium (ISM) at a high level of sensitivity,
where also faint point sources stand out and allow for the discovery
of PNe, Wolf-Rayet (WR) stars, etc. (3) The use of the P3D
line-fitting tool yields emission line fluxes, surface brightness, and
kinematic information for gaseous objects, corrected for absorption
line profiles of the underlying stellar population in the case of
Hα. (4) Visual inspection of the data cubes by browsing through
the row-stacked spectra image in P3D is demonstrated to be efficient
for data mining and the discovery of background galaxies and unusual
objects.
We present a catalog of luminous stars, rare stars such as WR, and
other emission line stars, carbon stars, symbiotic star candidates,
PNe, HII regions, SNR, giant shells, peculiar diffuse and
filamentary emission line objects, and background galaxies, along with
their spectra.
The technique of crowded-field 3D spectroscopy, using the PampelMUSE
code, is capable of deblending individual bright stars, the unresolved
background of faint stars, gaseous nebulae, and the diffuse component
of the ISM, resulting in unprecedented legacy value for observations
of nearby galaxies with MUSE.
Description:
Observations were made with the multi unit spectroscopic explorer
instrument (MUSE), which is placed at the Nasmyth focus of the UT4
8.2m telescope at the Very Large Telescope observatory (VLT) of the
European Southern Observatory (ESO) in Chile. NGC 300 was observed as
part of guaranteed time observations of the MUSE instrument-building
consortium during the three periods P93, P94, and P95.
We present a catalog of luminous stars, rare stars such as WR, and
other emission line stars, carbon stars, symbiotic star candidates,
PNe, HII regions, SNR, giant shells, peculiar diffuse and filamentary
emission line objects, and background galaxies, along with their
spectra.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 85 557 Catalog of stars in field (i) with spectral
type classification
table9.dat 92 118 Catalog of emission line stars in fields (a)-(j)
list.dat 98 1 Datacube informations
fits/* . 1 *Datacube
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Note on fits/*: the data cube field-i.fits can be conveniently visualized and
analyzed using the open source software P3D, available and fully documented
at https://p3d.sourceforge.io/
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See also:
J/A+A/306/9 : PNe and HII in NGC 300 (Soffner+, 1996)
J/AJ/123/789 : ARAUCARIA project: NGC300 Cepheid variables (Pietrzynski+ 2002)
J/AJ/128/1167 : ARAUCARIA project: NGC300 Cepheid Variables. II (Gieren+, 2004)
J/ApJ/789/81 : Multiwavelength survey of HII regions in NGC 300 (Faesi+, 2014)
J/A+A/547/A78 : Catalog of NGC 300 planetary nebula candidates (Pena+, 2012)
J/ApJ/758/15 : Chandra X-ray point sources of NGC 300 (Binder+, 2012)
Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 I6 --- ID Catalog number (1)
8- 12 F5.2 mag F606W HST ACS magnitude F606W
14- 15 I2 h RAh Right ascension (J2000.0)
17- 18 I2 min RAm Right ascension (J2000.0)
20- 23 F4.1 s RAs Right ascension (J2000.0)
25 A1 --- DE- Declination sign (J2000.0)
26- 27 I2 deg DEd Declination (J2000.0)
29- 30 I2 arcmin DEm Declination (J2000.0)
32- 35 F4.1 arcsec DEs Declination (J2000.0)
37- 40 F4.1 --- SNR Signal-to-noise ration per spectral bin
42 A1 --- B [0-8] Blending flag (2)
44- 48 I5 K Teff ?=0 Effective temperature of best fit (3)
50- 54 F5.2 [cm/s2] logg ?=9.99 Gravity of best fit (3)
56- 60 F5.2 --- [Fe/H] ?=9.99 Metallicity of best fit (3)
62- 64 I3 km/s RV ?=999 Radial velocity
66- 68 I3 km/s e_RV ?=999 Radial velocity error
70- 83 A14 --- SpType Spectral type of best fit
85 A1 --- Plaus [0-2] Plausibility flag of fit (4)
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Note (1): ID<200000 refer to stars with HST ACS coverage,
ID>200000 to stars outside the ACS field-of-view.
ID 1003 is a peculiar red star visible in HST image, that was however
not detected in MUSE data cube.
Note (2): Blending flag as follows:
0 = significant
1 = minor
2 = not obvious
8 = cluster
Note (3): "9.99" in columns log g and [Fe/H], and "999" in columns RV and
e_RV indicate uncertain results. "0" in column Teff indicates that no
satisfactory fit was obtained.
Note (4): Plausibility flag of fit as follows:
0 = uncertain
1 = marginal
2 = very plausible
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- ID Catalog number (aNNNa) (1)
6- 8 I3 --- PM ? Cross reference to PampelMuse ID
10- 15 F6.2 pix X Data cube x coordinate (RA)
17- 22 F6.2 pix Y Data cube y coordinate (DEC)
24- 25 I2 h RAh Right ascension (J2000.0)
27- 28 I2 min RAm Right ascension (J2000.0)
30- 35 F6.3 s RAs Right ascension (J2000.0)
37 A1 --- DE- Declination sign (J2000.0)
38- 39 I2 deg DEd Declination (J2000.0)
41- 42 I2 arcmin DEm Declination (J2000.0)
44- 48 F5.2 arcsec DEs Declination (J2000.0)
50- 52 F3.1 10-20W/m2 F(Hb) ? Hβ flux in 10e-17 erg/cm2/s
54- 56 F3.1 10-20W/m2 e_F(Hb) ? Hβ flux error in 10e-17 erg/cm2/s
58- 61 F4.1 10-20W/m2 F(Ha) ? Hα flux in 10e-17 erg cm2/s
63- 65 F3.1 10-20W/m2 e_F(Ha) ? Hα flux error in 10e-17 erg/cm2/s
67- 69 I3 km/s RV Radial velocity
71- 72 I2 km/s e_RV Radial velocity error
74- 76 F3.1 0.1nm FWHM ? Halpha emission line FWHM (Angstrom)
78 A1 --- wings [w] Extended Halpha wings, flag "w"
80- 84 A5 --- Q Quality flag (2)
86- 92 A7 --- Col Apparent colour of star flag (3)
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Note (1): the prefix "a"..."j" of ID refers to field (a) ... (j)
Note (2): Quality flag as follows:
conf. = confirmed
? = uncertain
no = no star seen, other emission emission line object
Note (3): Colour flag, for colours blues, red, and yel for yellow as follows:
-f = faint
-s = symbiotic star candidate
-c = carbon star
-wr = Wolf Rayet star
-? = uncertain
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Byte-by-byte Description of file: list.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 22 F3.1 arcsec/pix scale [0.2] Scale of the image
24- 26 I3 --- Nx [321] Number of pixels along X-axis
28- 30 I3 --- Ny [318] Number of pixels along Y-axis
32- 35 I4 --- Nz [3801] Number of slices
37- 43 F7.2 0.1nm blambda [4599.66] Lower value of wavelength interval
45- 51 F7.2 0.1nm Blambda [9349.66] Lower value of wavelength interval
53- 56 F4.2 0.1nm dlambda [1.25] Wavelength step
58- 64 I7 Kibyte size [1515628] Size of FITS file
66- 77 A12 --- FileName Name of FITS file, in subdirectory fits
79- 98 A20 --- Title Title of the FITS file
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Acknowledgements:
Martin M. Roth, mmroth(at)aip.de
(End) Martin M. Roth [AIP, Germany], Patricia Vannier [CDS] 05-Oct-2018