Access to Astronomical Catalogues

← Click to display the menu
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 (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; 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) ------------------------------------------------------------------ 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
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). 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)). 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) 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); 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). Note (6): Spectroscopic redshift References as follows: CG15 = Grillo et al. (2015ApJ...800...38G); GC16 = Caminha et al. (2016arXiv160703462C); IB15 = Balestra et al. (2016, J/ApJS/224/33); JR14 = Kneib et al. in prep.; LC12 = Christensen et al. (2012MNRAS.427.1953C; <[CRH2012] MACS J0416.1-2403 N.N> in Simbad); MJ14 = Jauzac et al. (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
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.
History: From electronic version of the journal References: Treu et al. Paper I. 2015ApJ...812..114T Cat. J/ApJ/812/114 Jones et al. Paper II. 2015AJ....149..107J Schmidt et al. Paper III. 2016ApJ...818...38S Wang et al. Paper IV. 2015ApJ...811...29W Cat. J/ApJ/811/29 Vulcani et al. Paper V. 2015ApJ...814..161V Hoag et al. Paper VI. 2016ApJ...831..182H This catalog Vulcani et al. Paper VII. 2016ApJ...833..178V Cat. J/ApJ/833/178 Vulcani et al. Paper VIII. 2017ApJ...837..126V Morishita et al. Paper IX. 2017ApJ...835..254M Cat. J/ApJ/835/254 Wang et al. Paper X. 2017ApJ...837...89W Schmidt et al. Paper XI. 2017ApJ...839...17S
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 13-Feb-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service