J/ApJ/831/182 GLASS. VI. MCS J0416.1-2403 HFF imaging & spectra (Hoag+, 2016)
The Grism Lens-Amplified Survey from Space (GLASS).
VI. Comparing the mass and light in MACS J0416.1-2403 using frontier field
imaging and GLASS spectroscopy.
Hoag A., Huang K.-H., Treu T., Bradac M., Schmidt K.B., Wang X.,
Brammer G.B., Broussard A., Amorin R., Castellano M., Fontana A.,
Merlin E., Schrabback T., Trenti M., Vulcani B.
<Astrophys. J., 831, 182-182 (2016)>
=2016ApJ...831..182H 2016ApJ...831..182H (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Gravitational lensing ; Spectroscopy ;
Redshifts ; Photometry, HST ; Infrared sources
Keywords: galaxies: clusters: individual: MACS J0416.1-2403;
gravitational lensing: strong
Abstract:
We present a model using both strong and weak gravitational lensing of
the galaxy cluster MACS J0416.1-2403, constrained using spectroscopy
from the Grism Lens-Amplified Survey from Space (GLASS) and Hubble
Frontier Fields (HFF) imaging data. We search for emission lines in
known multiply imaged sources in the GLASS spectra, obtaining secure
spectroscopic redshifts of 30 multiple images belonging to 15 distinct
source galaxies. The GLASS spectra provide the first spectroscopic
measurements for five of the source galaxies. The weak lensing signal
is acquired from 884 galaxies in the F606W HFF image. By combining the
weak lensing constraints with 15 multiple image systems with
spectroscopic redshifts and nine multiple image systems with
photometric redshifts, we reconstruct the gravitational potential of
the cluster on an adaptive grid. The resulting map of total mass
density is compared with a map of stellar mass density obtained from
the deep Spitzer Frontier Fields imaging data to study the relative
distribution of stellar and total mass in the cluster. We find that
the projected stellar mass to total mass ratio, f*, varies
considerably with the stellar surface mass density. The mean projected
stellar mass to total mass ratio is <f*≥0.009±0.003 (stat.), but
with a systematic error as large as 0.004-0.005, dominated by the
choice of the initial mass function. We find agreement with several
recent measurements of f* in massive cluster environments. The lensing
maps of convergence, shear, and magnification are made available to
the broader community in the standard HFF format.
Description:
The Grism Lens-Amplified Survey from Space (GLASS; GO-13459, PI: Treu;
Schmidt+ 2014ApJ...782L..36S 2014ApJ...782L..36S; Treu+ 2015, J/ApJ/812/114) observed 10
massive galaxy clusters with the HST WFC3-IR G102 and G141 grism
between 2013 December and 2015 January. Each of the clusters targeted
by GLASS has deep multi-band HST imaging from the Hubble Frontier
Fields (HFF) in 2014 September and/or from CLASH (ESO VIMOS large
program CLASH-VLT; 186.A-0798; PI: P. Rosati; Balestra+, 2016,
J/ApJS/224/33).
We also use mid-IR imaging data acquired with the IRAC on board the
Spitzer Space Telescope obtained by the DDT program #90258
(PI: Soifer; P. Capak+ 2016, in prep.) and #80168 (PI: Bouwens).
Objects:
------------------------------------------------------------------
RA (ICRS) DE Designation(s)
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04 16 10.0 -24 03 58 MACS J0416.1-2403 = MCS J0416.1-2403
------------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 133 272 Multiply lensed arc systems identified in
the MACSJ0416.1-2403 field
table3.dat 121 201 GLASS spectroscopic results for multiply and
singly lensed sources
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See also:
J/ApJS/224/33 : CLASH-VLT: the FF cluster MACS J0416.1-2403 (Balestra+, 2016)
J/ApJ/817/60 : Multiply imaged supernova Refsdal (Treu+, 2016)
J/A+A/590/A31 : ASTRODEEP Frontier Fields Catalogues (Merlin+, 2016)
J/ApJ/812/114 : Grism Lens-Amplified Survey from Space (GLASS) I. (Treu+, 2015)
J/ApJ/801/44 : HST lensing analysis of the CLASH sample (Zitrin+, 2015)
J/MNRAS/444/268 : HST Frontier Fields clusters (Richard+, 2014)
J/MNRAS/443/1549 : MACSJ0416.1-2403 strong-lensing analysis (Jauzac+, 2014)
J/ApJ/762/L30 : CLASH: MCS J0416.1-2403 strong lensing analysis (Zitrin+, 2013)
J/ApJ/660/239 : MaxBCG cat. of 13823 galaxy clusters from SDSS (Koester+, 2007)
J/AJ/132/926 : Galaxies in the Hubble Ultra Deep Field (Coe+, 2006)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- arcID ID of multiple image from lens modeling (1)
6 A1 --- f_arcID [ap] Flag on arcID (2)
8 I1 --- n_arcID [1/7]? Notes on arcID (3)
11- 15 I5 --- GLASSID [185/1403]? ID from the GLASS program (4)
17- 25 F9.6 deg RAdeg [64.02/64.06] Right ascension (J2000)
27- 36 F10.6 deg DEdeg [-24.1/-24] Declination (J2000)
38- 41 A4 --- Cref Coordinate References (5)
43- 48 F6.4 --- zspec1 [0.7/3.3]? Spectroscopic Redshift 1
50- 54 A5 --- r_zspec1 Reference for zspec1 (6)
56- 61 F6.4 --- zspec2 [1.6/3.3]? Spectroscopic Redshift 2
63- 66 A4 --- r_zspec2 Reference for zspec2 (6)
68- 71 F4.2 --- zgrism [0.9/2.4]? Grism redshift, this work (7)
73- 75 F3.1 --- zBayes [1/6.2]? Hierarchical Bayesian modeled
redshift (8)
79- 81 F3.1 --- E_zBayes [0.1/5.2]? Upper uncertainty on zBayes
86- 88 F3.1 --- e_zBayes [0.1/5]? Low uncertainty on zBayes
91- 95 F5.2 mag F140W [20.2/29.4]? HST/WFC3 IR F140W AB magnitude (9)
99-102 F4.2 mag e_F140W [0/0.6]? Uncertainty in F140Wmag
104-109 F6.2 --- mu [1.1/401.3]? Magnification (µ) (10)
112-117 F6.2 --- E_mu [0/485]? Upper uncertainty on mu (10)
120-125 F6.2 --- e_mu [0/311]? Lower uncertainty on mu (10)
128-133 A6 --- Set Sample
--------------------------------------------------------------------------------
Note (1): arcIDs for multiple image systems 19-22 are intentionally omitted for
consistency with IDs from the recent literature,
i.e., Jauzac+ 2014, J/MNRAS/443/1549; <[JCL2014] NN.N> in Simbad.
Objects starting with "D" are from Diego+ (2015MNRAS.447.3130D 2015MNRAS.447.3130D).
Note (2): Flag on arcID as follows:
p = Proposed multiple candidate which is less confident identification.
a = Alternative image to those with the same ID listed without "a".
Note (3): Notes on individual arcID as follows:
1 = Systems 3 and 4 are believed to be different substructures of the same
source galaxy due to the similar redshift and spatial position of the
multiple images in each system.
2 = The GLASS spectroscopic redshifts of arcIDs 5.1 and 5.4 were determined
after the HFF modeling procedure took place. Therefore, neither image
was included in the Gold sample.
3 = arcID 12.3 does not belong to the Gold sample despite our measurement
of zgrism=1.95 because it is still not known whether 12.3 is the
correct counter-image to 12.1 and 12.2, both of which lack
spectroscopic confirmation.
4 = The spectroscopic redshift of system 14 was reported erroneously by
Jauzac+ (2014, J/MNRAS/443/1549) at z=2.0531 using incomplete
CLASH-VLT data. We measured zgrism=1.63 for all three images in the
system, in agreement with the redshift obtained using the complete
CLASH-VLT data (I. Balestra, private communication, Grillo+
(2015ApJ...800...38G 2015ApJ...800...38G)).
5 = The redshift of this object was reported at zgrism=2.18±0.01 (Q=3)
in the original GLASS catalog based on two marginal emission lines,
but while preparing the manuscript Caminha et al. (2016arXiv160703462C 2016arXiv160703462C)
published a redshift of z=3.238 from bright Lyα, which ruled
out the grism redshift.
6 = Balestra+ (2016, J/ApJS/224/33) published their spectroscopic
redshifts after the HFF modeling teams graded the multiple images into
the Gold, Silver and Bronze categories. We include them in this table
for completeness and comparison with zgrism.
7 = 29.1 was originally assigned as a Gold image from GLASS spectroscopy,
but further analysis after the samples were chosen revealed that
the spectroscopic confirmation was too tenuous. Therefore, this
object should not be considered to be spectroscopically confirmed.
Note (4): Entries where GLASSID is blank had no match in the grism
detection image.
Note (5): Coordinate References as follows:
D15 = Diego et al. (2015MNRAS.447.3130D 2015MNRAS.447.3130D);
JPK = Kneib et al. in prep.;
MJ14 = Jauzac et al. (2014, J/MNRAS/443/1549; <[JCL2014] NN.N> in Simbad);
RK = Kawamata et al. in prep.;
TJ14 = Johnson et al. (2014ApJ...797...48J 2014ApJ...797...48J).
Note (6): Spectroscopic redshift References as follows:
CG15 = Grillo et al. (2015ApJ...800...38G 2015ApJ...800...38G);
GC16 = Caminha et al. (2016arXiv160703462C 2016arXiv160703462C);
IB15 = Balestra et al. (2016, J/ApJS/224/33);
JR14 = Kneib et al. in prep.;
LC12 = Christensen et al. (2012MNRAS.427.1953C 2012MNRAS.427.1953C;
<[CRH2012] MACS J0416.1-2403 N.N> in Simbad);
MJ14 = Jauzac et al. (2014MNRAS.443.1549J 2014MNRAS.443.1549J; <[JCL2014] NN.N> in Simbad);
SR14 = Rodney et al. in prep.
Note (7): Typical uncertainty on zgrism is 0.01, corresponding to a grism
wavelength uncertainty of ∼50 Angstroms.
Note (8): zBayes is the redshift obtained for a multiple image system from
hierarchical Bayesian modeling. zBayes (E_zBayes, e_zBayes≡95% conf.
limits) is only shown for systems with two or more reliable
photometric redshift measurements.
Note (9): Objects for which F140W magnitudes (68% conf. limits) are blank
are not detected in our photometric catalog.
Note (10): The magnification (E_Magn, e_Magn ≡ 68% conf. limits) was calculated
using the best-fit lens model scaled to the spectroscopic redshift of
the multiple image system, or zBayes if the spectroscopic redshift
was not known. Some multiple images have best-fit magnifications that
are outside of the 68% confidence interval due to non Gaussian error
distributions.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 I5 --- GLASSID [47/90016] ID from the GLASS program (1)
7- 15 A9 --- arcID ID of multiple image from lens modeling
17 A1 --- n_arcID [a-c] Notes on individual arcIDs (2)
19- 26 F8.5 deg RAdeg Right ascension in decimal degrees (J2000)
28- 36 F9.5 deg DEdeg Declination in decimal degrees (J2000)
38- 42 F5.2 mag F140W [17.9/27.2]? HST/WFC3 IR F140W AB magnitude
44- 47 F4.2 mag e_F140W [0/0.2]? Uncertainty in F140Wmag
49- 51 F3.1 --- zphot [0/7]? Photometric redshift (3)
53- 56 F4.1 --- E_zphot [0/6.1]? Upper uncertainty on zphot
58- 61 F4.1 --- e_zphot [0/6]? Lower uncertainty on zphot
63- 66 F4.2 --- zgrism [0.1/3.1]? Grism redshift
68 I1 --- q_zgrism [2/4]? Quality of zgrism (4=secure) (4)
70 I1 --- Nl [0/4] Number of emission lines detected
72- 98 A27 --- Lines List of emission lines detected
100-105 F6.2 --- mu [1/402]? Magnification (µ)
107-113 F7.2 --- E_mu [0/131]? Upper uncertainty on mu
116-121 F6.2 --- e_mu [0/311]? Lower uncertainty on mu
--------------------------------------------------------------------------------
Note (1): Objects with GLASSID in the format 9XXXX come from an extraction
based on a different source detection image than the one used to
extract the other GLASS IDs.
Note (2): Individual arcID notes as follows:
a = Systems 3 and 4 are believed to be different substructures of the
same source galaxy due to the similar redshift and spatial position
of the multiple images in each system;
b = The uncertainty in zgrism for arcID 12.3 is ∼0.02,
rather than the nominal ∼0.01 because the redshift was obtained by
fitting its continuum emission in the grism to SED templates rather
than through the identification of emission lines;
c = arcIDs 28.1 and 28.2 were detected as the same object
in the segmentation map used to extract the grism data.
Note (3): The images for which zphot is not shown are either contaminated or
not detected in the photometric catalog.
Note (4): Quality flag as follows:
4 = secure;
3 = probable;
2 = possible;
1 = likely an artifact.
See section 4.2 for further explanations.
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History:
From electronic version of the journal
References:
Treu et al. Paper I. 2015ApJ...812..114T 2015ApJ...812..114T Cat. J/ApJ/812/114
Jones et al. Paper II. 2015AJ....149..107J 2015AJ....149..107J
Schmidt et al. Paper III. 2016ApJ...818...38S 2016ApJ...818...38S
Wang et al. Paper IV. 2015ApJ...811...29W 2015ApJ...811...29W Cat. J/ApJ/811/29
Vulcani et al. Paper V. 2015ApJ...814..161V 2015ApJ...814..161V
Hoag et al. Paper VI. 2016ApJ...831..182H 2016ApJ...831..182H This catalog
Vulcani et al. Paper VII. 2016ApJ...833..178V 2016ApJ...833..178V Cat. J/ApJ/833/178
Vulcani et al. Paper VIII. 2017ApJ...837..126V 2017ApJ...837..126V
Morishita et al. Paper IX. 2017ApJ...835..254M 2017ApJ...835..254M Cat. J/ApJ/835/254
Wang et al. Paper X. 2017ApJ...837...89W 2017ApJ...837...89W
Schmidt et al. Paper XI. 2017ApJ...839...17S 2017ApJ...839...17S
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Feb-2017