J/ApJ/893/47 Milky Way satellite census. I. DES & PS1 (Drlica-Wagner+, 2020)
Milky Way satellite census.
I. The observational selection function for Milky Way satellites in DES y3 and
Pan-STARRS DR1.
Drlica-Wagner A., Bechtol K., Mau S., McNanna M., Nadler E.O., Pace A.B.,
Li T.S., Pieres A., Rozo E., Simon J.D., Walker A.R., Wechsler R.H.,
Abbott T.M.C., Allam S., Annis J., Bertin E., Brooks D., Burke D.L.,
Carnero Rosell A., Carrasco Kind M., Carretero J., Costanzi M.,
Da Costa L.N., De Vicente J., Desai S., Diehl H.T., Doel P., Eifler T.F.,
Everett S., Flaugher B., Frieman J., Garcia-Bellido J., Gaztanaga E.,
Gruen D., Gruendl R.A., Gschwend J., Gutierrez G., Honscheid K.,
James D.J., Krause E., Kuehn K., Kuropatkin N., Lahav O., Maia M.A.G.,
Marshall J.L., Melchior P., Menanteau F., Miquel R., Palmese A.,
Plazas A.A., Sanchez E., Scarpine V., Schubnell M., Serrano S.,
Sevilla-Noarbe I., Smith M., Suchyta E., Tarle G., (the DES Collaboration)
<Astrophys. J., 893, 47-47 (2020)>
=2020ApJ...893...47D 2020ApJ...893...47D (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way; Galaxies, photometry; Surveys; Magnitudes, absolute;
Photometry, UBV
Keywords: Dwarf spheroidal galaxies; Local Group; Dark matter; Milky Way Galaxy
Abstract:
We report the results of a systematic search for ultra-faint Milky Way
satellite galaxies using data from the Dark Energy Survey (DES) and
Pan-STARRS1 (PS1). Together, DES and PS1 provide multi-band photometry
in optical/near-infrared wavelengths over ∼80% of the sky. Our search
for satellite galaxies targets ∼25000deg2 of the
high-Galactic-latitude sky reaching a 10σ point-source depth of
≳22.5mag in the g and r bands. While satellite galaxy searches have
been performed independently on DES and PS1 before, this is the first
time that a self-consistent search is performed across both data sets.
We do not detect any new high-significance satellite galaxy
candidates, recovering the majority of satellites previously detected
in surveys of comparable depth. We characterize the sensitivity of our
search using a large set of simulated satellites injected into the
survey data. We use these simulations to derive both analytic and
machine-learning models that accurately predict the detectability of
Milky Way satellites as a function of their distance, size,
luminosity, and location on the sky. To demonstrate the utility of
this observational selection function, we calculate the luminosity
function of Milky Way satellite galaxies, assuming that the known
population of satellite galaxies is representative of the underlying
distribution. We provide access to our observational selection
function to facilitate comparisons with cosmological models of galaxy
formation and evolution.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 88 61 Confirmed and candidate Milky Way satellites
table3.dat 61 21 Recovery of confirmed and candidate Milky Way
satellite galaxies in DES Y3A2
table4.dat 61 32 Recovery of confirmed and candidate Milky Way
satellite galaxies in PS1 DR1
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See also:
VII/4 : Abell and Zwicky Clusters of Galaxies (Abell+ 1974)
VII/195 : Globular Clusters in the Milky Way (Harris, 1996)
VII/202 : Globular Clusters in the Milky Way (Harris, 1997)
VII/239 : History and Accurate Positions for the NGC/IC Objects (Corwin, 2004)
II/349 : The Pan-STARRS release 1 (PS1) Survey - DR1 (Chambers+, 2016)
II/357 : The Dark Energy Survey (DES): Data Release 1 (Abbott+, 2018)
J/MNRAS/389/678 : Extended objects in Magellanic Clouds (Bica+, 2008)
J/MNRAS/397/1748 : Spectroscopic study of Segue 2 (Belokurov+, 2009)
J/AJ/144/4 : Dwarf galaxies in the Local Group (McConnachie+, 2012)
J/ApJ/746/178 : The augmented maxBCG cluster catalog (Rykoff+, 2012)
J/ApJ/750/99 : The Pan-STARRS1 photometric system (Tonry+, 2012)
J/A+A/558/A53 : MW global survey of star clusters. II. (Kharchenko+, 2013)
J/ApJ/776/80 : PAndAS view of Andromeda satellites. I. (Martin+, 2013)
J/ApJ/780/59 : The Araucaria project: EBs in SMC (Graczyk+, 2014)
J/ApJ/789/147 : Star formation histories of LG dwarf galaxies (Weisz+, 2014)
J/ApJ/803/63 : gr photometry of stars in Kim 2 (Kim+, 2015)
J/ApJ/863/25 : Deep Megacam obs. of 4 MW satellites (Mutlu-Pakdil+, 2018)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Satellite identifier (1)
19- 26 A8 --- Survey Survey where system resides
28 I1 --- Class System classification number (2)
30- 37 F8.4 deg RAdeg Right Ascension in decimal degrees (J2000)
39- 46 F8.4 deg DEdeg Declination in decimal degrees (J2000)
48- 51 F4.1 mag m-M Published distance modulus
53- 58 F6.2 arcmin ah Semi-major axis (3)
60 A1 --- l_ell Limit flag on ell
61- 65 F5.2 --- ell Ellipticity; 1-b/a
67- 69 I3 kpc Dist Derived heliocentric distance
71- 74 I4 pc r1/2 Azimuthally averaged physical half-light radius
76- 81 F6.2 mag VMag Published absolute V band magnitude
83- 88 A6 --- Ref Literature reference code(s) (4)
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Note (1): Bootes III has its approximate half-light and ellipticity estimated
from Grillmair (2009ApJ...693.1118G 2009ApJ...693.1118G).
Note (2): Classification code as follows:
1 = unconfirmed systems (2 occurrences);
2 = probable star clusters (2 occurrences);
3 = probable dwarfs (18 occurrences);
4 = kinematically confirmed dwarfs (39 occurrences).
Note (3): Of an ellipse containing half of the light.
Note (4): When two references are listed, the second was used for the
distance measurement. Reference codes as follows:
1 = Torrealba et al. (2019MNRAS.488.2743T 2019MNRAS.488.2743T)
2 = Torrealba et al. (2016MNRAS.463..712T 2016MNRAS.463..712T)
3 = Munoz et al. (2018ApJ...860...66M 2018ApJ...860...66M)
4 = Grillmair et al. (2009ApJ...693.1118G 2009ApJ...693.1118G)
5 = Homma et al. (2019PASJ...71...94H 2019PASJ...71...94H)
6 = Torrealba et al. (2018MNRAS.475.5085T 2018MNRAS.475.5085T)
7 = Mau et al. (2020ApJ...890..136M 2020ApJ...890..136M)
8 = Drlica-Wagner et al. (2015ApJ...813..109D 2015ApJ...813..109D)
9 = Homma et al. (2018PASJ...70S..18H 2018PASJ...70S..18H)
10 = Carlin et al. (2017AJ....154..267C 2017AJ....154..267C)
11 = Torrealba et al. (2016MNRAS.459.2370T 2016MNRAS.459.2370T)
12 = Luque et al. (2017MNRAS.468...97L 2017MNRAS.468...97L)
13 = Longeard et al. (2018MNRAS.480.2609L 2018MNRAS.480.2609L)
14 = Pietrzynski et al. (2009AJ....138..459P 2009AJ....138..459P)
15 = Kim et al. (2015ApJ...808L..39K 2015ApJ...808L..39K)
16 = Koposov et al. (2018MNRAS.479.5343K 2018MNRAS.479.5343K)
17 = Makarov et al. (2014A&A...570A..13M 2014A&A...570A..13M)
18 = Pietrzynski et al. (2013Natur.495...76P 2013Natur.495...76P)
19 = Kim et al. (2016ApJ...833...16K 2016ApJ...833...16K)
20 = Drlica-Wagner et al. (2016ApJ...833L...5D 2016ApJ...833L...5D)
21 = Mcconnachie et al. (2012, J/AJ/144/4)
22 = Mutlu-Pakdil et al. (2018, J/ApJ/863/25)
23 = Martinez et al. (2015MNRAS.454.1509M 2015MNRAS.454.1509M)
24 = Graczyk et al. (2014, J/ApJ/780/59)
25 = Koposov et al. (2015ApJ...805..130K 2015ApJ...805..130K).
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Byte-by-byte Description of file: table[34].dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- Name Satellite identifier
19 A1 --- f_Name [ab] Flag on Name (1)
21 I1 --- Set Statistical sample code (2)
23- 28 F6.2 --- sqrtTS ? Square root of ugali search test
statistic (3)
30- 34 F5.2 --- Sig ? Statistical significance value from
simple search
36- 39 F4.2 --- Pdet Detection probability from survey
selection function
41- 43 I3 kpc Dist Derived heliocentric distance (4)
45- 48 I4 pc r1/2 Azimuthally averaged physical half-light
radius (4)
50- 55 F6.2 mag VMag Published absolute V band magnitude
57- 61 F5.2 arcmin-2 rho Local stellar density
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Note (1): Flag as follows:
a = Located in a masked region of the PS1 footprint (δ<-25deg).
b = Approximate half-light radius and ellipticity estimated from
Grillmair (2009ApJ...693.1118G 2009ApJ...693.1118G).
Note (2): Included in the statistical sample used to derive the luminosity
function: 1=True or 0=False.
Note (3): The ugali framework (Bechtol+ 2015ApJ...807...50B 2015ApJ...807...50B ;
Drlica-Wagner+ 2015ApJ...813..109D 2015ApJ...813..109D) employs a likelihood-based approach;
see Section 5.2.
Note (4): Calculated from observed parameters listed in Table 2.
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History:
From electronic version of the journal
References:
Nadler et al. Paper II. 2020ApJ...893...48N 2020ApJ...893...48N
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 09-Sep-2021