J/MNRAS/512/1091 NESS II Infrared and Sub-mm results (Scicluna+, 2022)
The Nearby Evolved Stars Survey II Constructing a volume-limited sample and
first results from the James Clerk Maxwell Telescope.
Scicluna P., Kemper F., Mcdonald I., Srinivasan S., Trejo A.,
Wallstrom S.H.J., Wouterloot J.G.A., Cami J., Greaves J., He J., Hoai D.T.,
Kim H., Jones O.C., Shinnaga H., Clark C.J.R., Dharmawardena T.,
Holland W., Imai H., Van Loon J.T., Menten K.M., Wesson R., Chawner H.,
Feng S., Goldman S., Liu F.C., Macisaac H., Tang J., Zeegers S., Amada K.,
Antoniou V., Bemis A., Boyer M.L., Chapman S., Chen X., Cho S.-H., Cui L.,
Dell'agli F., Friberg P., Fukaya S., Gomez H., Gong Y., Hadjara M.,
Haswell C., Hirano N., Hony S., Izumiura H., Jeste M., Jiang X.,
Kaminski T., Keaveney N., Kim J., Kraemer K.E., Kuan Y.-J., Lagadec E.,
Lee C.F., Li D., Liu S.-Y., Liu T., De Looze I., Lykou F., Maraston C.,
Marshall J.P., Matsuura M., Min C., Otsuka M., Oyadomari M., Parsons H.,
Patel N.A., Peeters E., Pham T.A., Qiu J., Randall S., Rau G., Redman M.P.,
Richards A.M.S., Serjeant S., Shi C., Sloan G.C., Smith M.W.L., Suh K.-W.,
Toala J.A., Uttenthaler S., Ventura P., Wang B., Yamamura I., Yang T.,
Yun Y., Zhang F., Zhang Y., Zhao G., Zhu M., Zijlstra A.A.
<Mon. Not. R. Astron. Soc. 512, 1091-1110 (2022)>
=2022MNRAS.512.1091S 2022MNRAS.512.1091S (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Stars, nearby ; Mass loss ; Interstellar medium ;
Infrared ; Millimetric/submm sources ; Photometry ;
Stars, distances ; Spectral types ; Positional data
Keywords: catalogues - surveys - stars: AGB and post-AGB - stars: mass-loss -
stars: winds, outflows
Abstract:
The Nearby Evolved Stars Survey (NESS) is a volume-complete sample of
∼850 Galactic evolved stars within 3 kpc at (sub-)mm wavelengths,
observed in the CO J = (2-1) and (3-2) rotational lines, and the
sub-mm continuum, using the James Clark Maxwell Telescope and Atacama
Pathfinder Experiment. NESS consists of five tiers, based on distances
and dust-production rate (DPR). We define a new metric for estimating
the distances to evolved stars and compare its results to Gaia EDR3.
Replicating other studies, the most-evolved, highly enshrouded objects
in the Galactic Plane dominate the dust returned by our sources, and
we initially estimate a total DPR of 4.7 * 10-5 M☉ yr-1 from
our sample. Our sub-mm fluxes are systematically higher and spectral
indices are typically shallower than dust models typically predict.
The 450/850 µm spectral indices are consistent with the blackbody
Rayleigh-Jeans regime, suggesting a large fraction of evolved stars
have unexpectedly large envelopes of cold dust.
Description:
This paper introduces the Nearby Evolved Stars Survey NESS, a
volume-complete statistically representative set of AGB stars in the
solar neighbourhood. Evolved stars are typically analysed using two
tracers, dust and molecular lines as CO lines. NESS aims to build a
coherent picture of mass-loss rates, by comparing these two mass
tracers. By making this selection, the NESS project is performing a
wide survey of a large number of AGB stars, ∼850, albeit at the cost
of recovering limited spatial information about the envelope of each
one. This places NESS as the widest project, with strong synergies to
other, ongoing large observing programmes. NESS aims to study the rate
and properties of the enriched matter returned to the ISM by evolved
stars and explore the physics of dust-laden stellar winds,
particularly their onset and time evolution.
As explained in the section 2.3.2 Object selection, we select 852
consistent IRAS sources in our final sample. Next, we fit 2MASS and
IRAS photometry sources with GRAMS model in order to extract
dust-production rates. We present these detailed results in the
table1.dat. Hereafter, we provide results from Sub-mm SCUBA-2
photometric observations of 138 objects. These observation results are
regrouped in the table3.dat.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 311 852 Physical properties of our NESS sources sample
table3.dat 164 138 Continuum fluxes and spectral indices from the
initial reduction of the SCUBA-2 data
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See also:
J/ApJS/112/557 : Classification of IRAS Sources (Kwok+ 1997)
J/A+A/532/A54 : GRAMS carbon-star model grid (Srinivasan+, 2011)
J/MNRAS/471/770 : Parameters and IR excesses of Gaia DR1 stars (McDonald+,2017)
J/ApJ/877/49 : DUSTiNGS. V. 3.6 and 4.5um light curves (Goldman+, 2019)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
J/AJ/156/112 : Near-infrared Mira period-luminosity relations in M33
(Yuan+, 2018)
J/ApJ/857/67 : HST obs. of Mira candidates in NGC 4258 (Huang+, 2018)
J/A+A/556/A38 : Period-mass-loss rate relation of Miras (Uttenthaler, 2013)
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/A+A/606/A67 : Circumstellar envelopes CO photodissociation
(Groenewegen, 2017)
J/ApJ/851/152 : DUSTiNGS. IV. AGB spectral types with HST (Boyer+, 2017)
J/ApJ/800/51 : DUSTiNGS II. Metal-poor dusty AGB stars (Boyer+, 2015)
J/AJ/142/103 : Cool evolved stars in SAGE-SMC and SAGE-LMC (Boyer+, 2011)
J/A+A/622/A120 : Mass loss from Miras with and without Tc (Uttenthaler, 2019)
https://evolvedstars.space/catalogue/ : current NESS catalogue
https://nida.esac.esa.int/nida-cl-web/?ACTION=OBSERVATION : ISO data archive
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- IRAS IRAS PSC identifier (IRASPSC)
13- 36 A24 --- SIMBAD SIMBAD main identifier (ID_SIM)
38- 53 A16 --- 2MASS 2MASS PSC designation (TMASS_Designation)
55- 66 A12 --- Tier NESS sample tier (sample) (1)
68 I1 --- Map [0/1] Whether source was mapped, yes for
46 sources (mapping) (2)
70- 86 F17.15 kpc D Distance estimate to source (DIST_BEST)
88- 110 E23.17 kpc e_D ? Uncertainty in distance estimate
(EDIST_BEST)
112- 116 A5 --- n_D [M H G L] Source of distance estimate
(DISTBESTTYPE) (3)
118- 125 I8 --- ISO ? Infrared Space Observatory ISO
identifier (ISO_TDT)
127 A1 --- LRS Spectroscopic IRAS LRS classification from
Kwok et al.
(1997ApJS..112..557K 1997ApJS..112..557K, Cat. J/ApJS/112/557)
(LRS_class)
129- 135 A7 --- SWS Spectroscopic ISO SWS classification from
Kraemer et al. (2002ApJS..140..389K 2002ApJS..140..389K)
(SWS_class)
137 A1 --- Chem [O S C]? Chemical type from spectrum
(spec_chemtype) (4)
139- 160 E22.17 Msun/yr dM/dt GRAMS best-fit dust-production rate DPR
(GRAMS_DPR) (5)
162- 183 E22.17 Msun/yr e_dM/dt Uncertainty in GRAMS best-fit DPR
(GRAMS_eDPR)
185 A1 --- ChemGram [o c] GRAMS best-fit chemical type
(GRAMS_chemtype) (6)
187- 209 F23.20 Jy Ftot450 GRAMS star+dust flux prediction at 450 um
(GRAMSftot450)
211- 231 E21.16 Jy Ftot850 GRAMS star+dust flux prediction at 850 um
(GRAMSftot850)
233- 252 F20.16 deg RAdeg Right ascension from simbad (J2000)
(RA_SIM)
254- 273 F20.16 deg DEdeg Declination from simbad (J2000) (DEC_SIM)
275- 291 F17.13 deg RAIdeg Right ascension from IRAS (J2000) (RA_IRAS)
293- 311 F19.15 deg DEIdeg Declination from IRAS (J2000) (DEC_IRAS)
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Note (1): As detailed in the section 2.3.4 Staring sample, five subsamples of
sources to be observed as follows:
very low = Tier 0, 19 very low dust-production rate (DPR) sources
low = Tier 1, 105 low DPR sources
intermediate = Tier 2, 222 intermediate DPR sources
high = Tier 3, 324 high DPR sources
extreme = Tier 4, 182 extremly high DPR sources
Note (2): As defined in the section 2.3.3 Determining preliminary mass-loss
rates and in section 2.3.5 Mapping sample, our source lists are
additionally divided into two groups, a large set to be observed in
spatially unresolved modes (the 'staring' sample) and a smaller group
to be mapped in detail (the 'mapping' sample).
Note (3): Sources of distance estimate are as follows:
M = Maser parallax observations, 9 objects in our sample
L = Luminosity distance measurements, 643 objects in our sample
H = Hipparcos parallax measurements, 193 objects in our sample
G = Tycho-Gaia Astrometric Solution of Gaia DR1, 7 objects in our
sample
Note (4): Chemical type from spectrum as follows:
O = O-rich oxygen rich stars, 494 objects in our sample
S = S-type star, 16 objects in our sample
C = C-rich star, 94 objects in our sample
Note (5): We fit the matched photometry in the 2MASS J, H, and Ks bands and the
IRAS 12, 25, and 60 µm bands with models from the Grid of Red
supergiant and AGB ModelS (GRAMS; Sargent et al. 2011ApJ...728...93S 2011ApJ...728...93S
and Srinivasan et al. 2011A&A...532A..54S 2011A&A...532A..54S, Cat. J/A+A/532/A54).
Note (6): GRAMS best-fit chemical type as follows:
o = o-rich oxygen stars, 758 objects in our sample
c = c-rich star, 94 objects in our sample
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- IRAS IRAS PSC identifier (IRASPSC)
12- 30 F19.14 Jy F450 JCMT/SCUBA2 450 um flux (SCUBA2_F450) (1)
32- 50 F19.15 Jy e_F450 Uncertainty in JCMT/SCUBA2 450 um flux
(SCUBA2F450err)
52- 53 I2 --- l_F450 [-1/0] JCMT/SCUBA2 450 um flux quality
flag, -1 if flux is 3σ upper limit,
42 cases in our sample (SCUBA2F450qual)
55- 73 F19.15 Jy F850 JCMT/SCUBA2 850 um flux (SCUBA2_F850) (1)
75- 93 F19.16 Jy e_F850 Uncertainty in JCMT/SCUBA2 850 um flux
(SCUBA2F850err)
95- 96 I2 --- l_F850 [-1/0] JCMT/SCUBA2 850 um flux quality
flag, -1 if flux is 3σ upper limit,
38 cases in our sample (SCUBA2F850qual)
98- 118 F21.18 --- alpha ? Spectral index see Section 4.4 Anomalous
detection of cold dust (alpha)
120- 139 F20.16 --- CIalphalow ? Lower bound of 68% confidence interval
for spectral index (alphacilow)
141- 160 F20.17 --- CIalphahigh ? Upper bound of 68% confidence interval
for spectral index (alphacihi)
162- 164 I3 --- q_alpha [-99/1] Quality flag for confidence
interval (-99, 0, 1) (alphaciqual)
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Note (1): Limits correspond to 3 times the RMS of the map in mJy/beam.
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History:
From electronic version of the journal
References:
Dharmawardena et al., Paper I 2019MNRAS.489.3218D 2019MNRAS.489.3218D
(End) Luc Trabelsi [CDS] 07-Mar-2025