J/A+A/704/A276 Nearby Evolved Stars Survey. III. (Wallstroem+, 2025)
The Nearby Evolved Stars Survey.
III: First data release of JCMT CO-line observations.
Wallstroem S.H.J., Scicluna P., Srinivasan S., Wouterloot J.G.A.,
McDonald I., Decock L., Wijshoff M., Chen R., Torres D., Umans L.,
Willebrords B., Kemper F., Rau G., Feng S., Jeste M., Kaminski T., Li D.,
Liu F.C., Trejo-Cruz A., Chawner H., Goldman S., MacIsaac H., Tang J.,
Zeegers S.T., Danilovich T., Matsuura M., Menten K.M., van Loon J.T.,
Cami J., Clark C.J.R., Dharmawardena T.E., Greaves J., He J., Imai H.,
Jones O.C., Kim H., Marshall J.P., Shinnaga H., Wesson R.,
the NESS Collaboration
<Astron. Astrophys. 704, A276 (2025)>
=2025A&A...704A.276W 2025A&A...704A.276W (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Stars, nearby ; Radio sources ; Carbon monoxide
Keywords: stars: AGB and post-AGB - stars: carbon - circumstellar matter -
stars: evolution - stars: mass-loss
Abstract:
Low- to intermediate-mass (∼0.8-8M☉) evolved stars contribute
significantly to the chemical enrichment of the interstellar medium in
the local Universe. It is therefore crucial to accurately measure the
mass return in their final evolutionary stages. The Nearby Evolved
Stars Survey (NESS) is a large multi-telescope project targeting a
volume-limited sample of ∼850 stars within 3kpc in order to
derive the dust and gas return rates in the solar neighbourhood, and
to constrain the physics underlying these processes. We present an
initial analysis of the CO-line observations, including detection
statistics, carbon isotopic ratios, initial mass-loss rates, and
gas-to-dust ratios. We describe a new data reduction pipeline for
homogeneity, which we use to analyse the available NESS CO data from
the James Clerk Maxwell Telescope, measuring line parameters and
calculating empirical gas mass-loss rates. We present the first
release of the available data on 485 sources, one of the largest
homogeneous samples of CO data to date. Comparison with a large
combined literature sample finds that high mass-loss rate and
especially carbon-rich sources are over-represented in literature,
while NESS is probing significantly more sources at low mass-loss
rates, detecting 59 sources in CO for the first time and providing
useful upper limits on non- detections. CO line detection rates are
81% for the CO (2-1) line and 75% for CO (3-2). The majority (82%) of
detected lines conform to the expected soft parabola shape, while
eleven sources show a double wind. Calculated mass-loss rates show
power-law relations with both the dust-production rates and expansion
velocities, up to a mass-loss rate saturation value
∼5x10-6M☉/yr. Median gas-to-dust ratios of 250 and 680 are
found for oxygen-rich and carbon-rich sources, respectively. Our
analysis of CO observations in this first data release highlights the
importance of our volume-limited approach in characterizing the local
AGB population as a whole.
Description:
This table contains JCMT observations of CO (2-1) and (3-2) rotational
lines for targets selected from the Nearby Evolved Stars Survey (NESS;
Paper II, Scicluna et al. 2022MNRAS.512.1091S 2022MNRAS.512.1091S, Cat. J/MNRAS/512/1091).
The table also contains the values for various parameters estimated
from these observations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablec1.dat 319 485 *CO observations and estimated parameters
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Note on tablec1.dat: All peak intensities, expansion velocities, and the related
uncertainties in the table are estimated from soft-parabola fits. Integrated
intensities are derived from the spectrum, not from the models.
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See also:
J/MNRAS/512/1091 : NESS II. Infrared and Sub-mm results (Scicluna+, 2022)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IRASPSC IRAS PSC identifier (IRASPSC)
13- 36 A24 --- SIMBADID SIMBAD identifier (SIMBAD_ID)
38 A1 --- Chemtype [O/C] Chemical type based on mid-IR
spectra [O for O-rich, C for C-rich];
see Section 2.4 (Chem_type)
40- 51 A12 --- Tier Grouping from Scicluna et al.
(2022MNRAS.512.1091S 2022MNRAS.512.1091S,) based on
location in distance-DPR space
(very low, low, intermediate, high,
or extreme) (Tier)
53- 59 F7.2 K PeakCO(2-1) ?=-999 Peak intensity of the CO(2-1)
line (Peak_CO(2-1))
61- 67 F7.2 K e_PeakCO(2-1) ?=-999 Uncertainty in the peak
intensity of the CO(2-1) line
(PeakCO(2-1)error)
69- 75 F7.2 km/s vinfCO(2-1) ?=-999 Expansion velocity of the
shell derived from the CO(2-1) line
(uncertainty 1km/s) (vinfCO(2-1))
77- 83 F7.2 K.km/s IntCO(2-1) ?=-999 Integrated intensity of the
CO(2-1) line (Int_CO(2-1))
85- 91 F7.2 K.km/s e_IntCO(2-1) []?=-999 Uncertainty in the integrated
intensity of the CO(2-1) line
(IntCO(2-1)error)
93- 96 I4 --- NchanCO(2-1) ?=-999 Number of velocity channels in
the CO(2-1) spectral band
(nchan_CO(2-1))
98-104 F7.2 K CO(2-1)rms ?=-999 RMS noise in the CO(2-1) line
(CO(2-1)_rms)
106-112 F7.2 K.km/s Int13CO(2-1) ?=-999 Integrated intensity of the
13CO(2-1) line (Int_13CO(2-1))
114-120 F7.2 K.km/s e_Int13CO(2-1) ?=-999 Uncertainty in the integrated
intensity of the 13CO(2-1) line
(Int13CO(2-1)error)
122-128 F7.2 K PeakCO(3-2) ?=-999 Peak intensity of the CO(3-2)
line (Peak_CO(3-2))
130-136 F7.2 K e_PeakCO(3-2) ?=-999 Uncertainty in the peak
intensity of the CO(3-2) line
(PeakCO(3-2)error)
138-144 F7.2 km/s vinfCO(3-2) ?=-999 Expansion velocity of the shell
derived from the CO(3-2) line
(uncertainty 1km/s) (vinfCO(3-2))
146-152 F7.2 K.km/s IntCO(3-2) ?=-999 Integrated intensity of the
CO(3-2) line (Int_CO(3-2))
154-160 F7.2 K.km/s e_IntCO(3-2) []?=-999 Uncertainty in the integrated
intensity of the CO(3-2) line
(IntCO(3-2)error)
162-165 I4 --- NchanCO(3-2) ?=-999 Number of velocity channels in
the CO(3-2) spectral band
(nchan_CO(3-2))
167-173 F7.2 --- CO(3-2)rms ?=-999 RMS noise in the CO(3-2) line
(CO(3-2)_rms)
175-181 F7.2 K.km/s Int13CO(3-2) ?=-999 Integrated intensity of the
13CO(3-2) line (Int_13CO(3-2))
183-189 F7.2 K.km/s e_Int13CO(3-2) ?=-999 Uncertainty in the integrated
intensity of the 13CO(3-2) line
(Int13CO(3-2)error)
191-200 E10.5 Msun/yr MLRCO(2-1) ?=- Empirical mass-loss rate derived
from the CO(2-1) line using the
Ramstedt et al. (2008A&A...487..645R 2008A&A...487..645R)
formula (MLR_CO(2-1))
202-211 E10.5 Msun/yr e_MLRCO(2-1) ?=- Uncertainty in the mass-loss
rate derived from the CO(2-1) line
(MLRCO(2-1)error)
213 I1 --- f_CO(2-1) [0/1] Flag designating whether the
CO(2-1) line is detected (0) or is
below 3 times the RMS (1)
(CO(2-1)_upperlimit)
215-224 E10.5 Msun/yr MLRCO(3-2) ?=- Empirical mass-loss rate derived
from the CO(3-2) line using the
Ramstedt et al. (2008A&A...487..645R 2008A&A...487..645R)
formula (MLR_CO(3-2))
226-235 E10.5 Msun/yr e_MLRCO(3-2) ?=- Uncertainty in the mass-loss rate
derived from the CO(3-2) line
(MLRCO(3-2)error)
237 I1 --- f_CO(3-2) [0/1] Flag denoting whether the CO(3-2) line
is detected (0) or is below 3 times
the RMS (1) (CO(3-2)_upperlimit)
239-243 F5.2 Msun/yr IsoRatio(2-1) Isotopic ratio 12CO/13CO derived from
the (2-1) lines (IsoRatio(2-1))
245-249 F5.2 Msun/yr IsoRatio(3-2) Isotopic ratio 12CO/13CO derived from
the (3-2) lines (IsoRatio(3-2))
251-260 E10.5 --- DPR Dust-production rate from SED fit
(DPR)
261-270 E10.5 --- e_DPR Uncertainty in the dust-production
rate (DPR_error)
271-277 F7.2 --- GasDustCO(2-1) ?=- Gas-to-dust ratio derived from the
CO(2-1) line (GasDust_CO(2-1))
279-285 F7.2 --- e_GasDustCO(2-1) ?=- Uncertainty in the gas-to-dust
ratio derived from the CO(2-1) line
(GasDustCO(2-1)error)
287-294 F8.2 --- GasDustCO(3-2) ?=- Gas-to-dust ratio derived from the
CO(3-2) line (GasDust_CO(3-2))
296-303 F8.2 --- e_GasDustCO(3-2) ?=- Uncertainty in the gas-to-dust
ratio derived from the CO(3-2) line
(GasDustCO(3-2)error)
305-308 I4 --- SoftParaCO(2-1) ?=-999[0/1] Flag denoting whether the
CO(2-1) line shape is a soft parabola
(1) or not (0) (SoftParabola_CO(2-1))
310-313 I4 --- SoftParaCO(3-2) ?=-999[0/1] Flag denoting whether the
CO(3-2) line shape is a soft parabola
(1) or not (0) (SoftParabola_CO(3-2))
315 I1 --- OptThin12CO(2-1) [0/1] Flag denoting whether the
CO(2-1) line is optically thin (1)
or not (0) (OptThin_12CO(2-1))
317 I1 --- OptThin12CO(3-2) [0/1] Flag denoting whether the
CO(3-2) line is optically thin (1)
or not (0) (OptThin_12CO(3-2))
319 I1 --- FirstDet [0/1] Flag denoting whether the NESS
observation is the first CO detection
for the source (1) or not (0)
(First_det)
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Acknowledgements:
Sundar Srinivasan, s.srinivasan(at)irya.unam.mx
References:
Dharmawardena et al., Paper I 2019MNRAS.489.3218D 2019MNRAS.489.3218D
Scicluna et al., Paper II 2022MNRAS.512.1091S 2022MNRAS.512.1091S, Cat. J/MNRAS/512/1091
(End) Sundar Srinivasan [IRyA-UNAM], Patricia Vannier [CDS] 14-Nov-2025