A refined mass distribution of the cluster MACS J0416.1−2403 from a new large set of spectroscopic multiply lensed sources

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Volume 600 (April 2017)

A&A, 600 (2017) A90

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Table A.1

Information on spectroscopically identified multiple images in MACS 0416.

ID	RA	Dec	z_MUSE	z_previous	ID_ref	mag_F814W

1a	64.049084	−24.062862	3.2355	–	26.3	27.87 ± 0.13
1b	64.046959	−24.060797	3.2355	–	26.2	27.43 ± 0.09
1c	64.046449	−24.060397	3.2355	2.185^a	26.1	26.53 ± 0.06

2a	64.050865	−24.066538	6.1452	–	207.2	28.20 ± 1.09 ^*
2b	64.048179	−24.062406	6.1452	–	–	29.06 ± 1.09 ^*
2c	64.043572	−24.059004	6.1452	–	206.1	28.66 ± 1.09 ^*

3a	64.049232	−24.068174	3.2885	–	44.3	27.50 ± 0.11
3b	64.045269	−24.062763	3.2885	–	44.1	25.69 ± 0.05
3c	64.041556	−24.059997	3.2885	–	44.2	26.13 ± 0.06

4a	64.048126	−24.066957	–	–	27.1	25.73 ± 0.03
4b	64.047468	−24.066039	–	2.107^a	27.2	24.13 ± 0.03
4c	64.042209	−24.060541	–	–	27.3	25.81 ± 0.04

5a	64.047463	−24.068822	1.8950	1.893^d^e^f	2.3	–
5b	64.043071	−24.063080	1.8950	1.893^d^e^f	2.2	23.88 ± 0.01 ^*
5c	64.041089	−24.061806	1.8950	1.893^d^e^f	2.1	23.67 ± 0.01 ^*

6a	64.047808	−24.070164	3.6065	–	–	28.53 ± 0.23
6b	64.043657	−24.064401	3.6065	–	–	26.73 ± 0.20
6c	64.037676	−24.060756	3.6065	–	–	28.00 ± 0.17

7a	64.047098	−24.071105	–	2.085^d^e^f	7.3	28.05 ± 0.14
7b	64.040664	−24.063586	2.0881	2.085^d^e^f	7.2	25.29 ± 0.03
7c	64.039795	−24.063081	2.0881	2.085^d^e^f	7.1	25.43 ± 0.04

8a	64.044624	−24.071488	–	2.282^a	29.3	25.81 ± 0.06
8b	64.040485	−24.066330	–	2.267^b	29.2a	–
8c	64.034256	−24.062997	–	–	29.1	25.76 ± 0.05

9a	64.045112	−24.072341	3.2882	–	32.1	26.11 ± 0.05 ^*
9b	64.040079	−24.066738	3.2882	–	32.2	25.33 ± 0.04 ^*
(9c)	(64.033157)	(−24.062893)	–	–	–	–

10a	64.044564	−24.072092	–	2.094^a	23.1	24.92 ± 0.02
10b	64.039576	−24.066623	–	–	23.2	25.20 ± 0.03
10c	64.034336	−24.063734	–	2.091^a	23.3	25.23 ± 0.03

(11a)	(64.046676)	(−24.075312)	–	–	–	–
11b	64.038515	−24.065965	3.2922	–	55.3	–
11c	64.035223	−24.064731	3.2922	–	55.1	27.93 ± 0.11

(12a)	(64.041365)	(−24.070852)	0.9397	–	28.3	–
12b	64.036843	−24.067457	0.9397	0.937^a	28.2	–
12c	64.036507	−24.067028	0.9397	0.937^a	28.1	–

13a	64.039245	−24.070383	1.0054	1.005^c	11.1	–
13b	64.038301	−24.069728	1.0054	1.005^c	11.2	–
13c	64.034234	−24.066016	1.0054	–	11.3	26.79 ± 0.12

14a	64.034483	−24.066956	3.2215	–	D22.1	–
14b	64.034190	−24.066488	3.2215	–	D22.2	–
14c	64.034001	−24.066445	3.2215	–	D22.3	–
(14d)	(64.045886)	(−24.076722)	–	–	–	–
(14e)	(64.035165)	(−24.067968)	–	–	–	–

15a	64.041802	−24.075731	1.9894	1.989^d^e^f	3.3	23.99 ± 0.01
15b	64.035249	−24.070989	1.9894	1.989^d^e^f	3.2	23.94 ± 0.02
15c	64.030769	−24.067129	1.9894	1.989^d^e^f	3.1	24.17 ± 0.01

16a	64.033523	−24.069448	2.0948	–	5.3	24.11 ± 0.02
16b	64.032656	−24.068663	2.0948	2.092^b	5.2	24.75 ± 0.02
16c	64.032410	−24.068414	2.0948	–	5.1	–
(16e)	(64.043470)	(−24.076860)	–	–	–	–

17a	64.040489	−24.078380	3.9663	–	–	27.97 ± 0.27
17b	64.035107	−24.073864	–	–	–	25.29 ± 0.17^∗
17c	64.027171	−24.068224	–	–	–	27.47 ± 0.17^∗

18a	64.040177	−24.079872	3.8710	–	49.2	27.12 ± 0.09
18b	64.033937	−24.074565	3.8710	–	49.1	27.08 ± 0.15
(18c)	(64.026991)	(−24.069620)	–	–	–	–

19a	64.040140	−24.080305	4.1032	–	51.1	26.70 ± 0.08 ^*
19b	64.033667	−24.074762	4.1032	–	51.2	25.38 ± 0.11 ^*
19c	64.026633	−24.070476	4.1032	–	51.3	–

20a	64.040351	−24.081482	–	3.223^d^e^f	13.3	25.75 ± 0.03
20b	64.032157	−24.075108	3.2175	3.223^d^e^f	13.2	–
20c	64.027572	−24.072673	3.2175	3.223^d^e^f	13.1	24.64 ± 0.02

(21a)	(64.042028)	(−24.081835)	–	–	–	–
21b^†	64.030906	−24.074341	5.1060	–	34.2	–
21c^†	64.029176	−24.073382	5.1060	–	34.1	–

(22a)	(64.040114)	(−24.082217)	–	–	–	–
22b	64.030997	−24.077173	3.9230	–	60.3	–
22c	64.027127	−24.073572	3.9230	–	–	29.54 ± 0.43

23a	64.035668	−24.079920	2.5425	2.545^b	45.1	26.27 ± 0.05
23b	64.032638	−24.078508	2.5425	–	–	–
(23c)	(64.024668)	(−24.071076)	–	–	–	–

24a	64.035833	−24.081321	1.6333	1.637^d	14.3	23.19 ± 0.01
24b	64.031039	−24.078953	1.6333	1.637^d	14.2	23.34 ± 0.01
24c	64.026239	−24.074337	1.6333	1.637^d	14.1	23.41 ± 0.01

25a	64.038073	−24.082404	3.1103	–	67.1	27.84 ± 0.13 ^*
25b	64.030366	−24.079015	3.1103	–	67.3	–
25c	64.025446	−24.073648	3.1103	–	67.2	28.06 ± 0.13

26a	64.037722	−24.082388	3.0773	–	58.2	27.58 ± 0.09
26b	64.030484	−24.079222	3.0773	–	58.3	26.49 ± 0.08
26c	64.025186	−24.073575	3.0773	–	58.1	27.46 ± 0.08

27a	64.037469	−24.083657	3.4909	–	35.1	–
27b	64.029409	−24.079889	3.4909	–	35.2	26.37 ± 0.05
27c	64.024946	−24.075021	3.4909	–	35.3	26.43 ± 0.04

28a	64.038350	−24.084126	–	–	–	28.76 ± 0.26
28b	64.028322	−24.079004	3.2526	–	47.2	–
28c	64.026330	−24.076705	3.2526	–	47.1	25.93 ± 0.05

29a	64.036702	−24.083855	–	2.298^d^e^f	10.3	25.60 ± 0.03
29b	64.028504	−24.079755	–	2.298^d^e^f	10.2	24.99 ± 0.02
29c	64.025993	−24.077080	–	2.298^d^e^f	10.1	24.57 ± 0.02

30a	64.033628	−24.083185	3.4406	–	38.1	27.20 ± 0.08
30b	64.031251	−24.081904	3.4406	–	38.2	26.98 ± 0.10 ^*
30c	64.022699	−24.074595	3.4406	–	38.3	27.94 ± 0.14 ^*

31a	64.035486	−24.084679	4.1218	–	48.1	26.21 ± 0.08
31b	64.029234	−24.081813	4.1218	–	48.2	24.76 ± 0.06 ^*
31c	64.023412	−24.076125	4.1218	–	48.3	25.39 ± 0.06

32a	64.035054	−24.085504	5.3650	–	33.2	27.95 ± 1.09
32b	64.028403	−24.082993	5.3650	–	33.1	26.60 ± 0.70 ^*
32c	64.022988	−24.077265	5.3650	–	33.2	26.03 ± 0.20 ^*

33a	64.032017	−24.084230	5.9729	–	–	27.03 ± 0.82 ^*
33b	64.030821	−24.083697	5.9729	–	–	–
(33c)	(64.021697)	(−24.075230)	–	–	–	–

(34a)	(64.034067)	(−24.085284)	–	–	–	–
34b	64.027632	−24.082609	3.9228	–	–	27.57 ± 0.28
34c	64.023731	−24.078477	3.9228	–	–	28.19 ± 0.45

35a^†	64.033681	−24.085855	5.6390	–	–	–
35b^†	64.028654	−24.084240	5.6390	–	–	–
35c^†	64.022187	−24.077559	5.6390	–	–	–

36a	64.031614	−24.085762	–	1.964^d^e	16.3	24.35 ± 0.02
36b	64.028339	−24.084553	–	1.964^d^e	16.2	23.48 ± 0.02
36c	64.024074	−24.080895	1.9614	1.964^d^e	16.1	–

37a	64.029809	−24.086363	–	2.218^d^e^f	17.1	24.32 ± 0.01
37b	64.028610	−24.085973	–	2.218^d^e^f	17.2	–
37c	64.023345	−24.081580	2.2182	2.218^d^e^f	17.3	–

Notes. IDs_ref corresponds to the ID column in Table 2 of Hoag et al. (2016). The F814W magnitudes are based on the ASTRODEEP catalog (Castellano et al. 2016). Model-predicted positions are indicated in brackets. MUSE redshifts are generally based on the Ly-α line when present, with exception of IDs 1, 3, 9, 20, 26, and 27 for which CIV and CIII] lines were used to better estimate the systemic redshift. This table includes 56 new redshifts belonging to 22 multiply lensed sources.

^(†)

Positions measured in MUSE narrow band images;

^(a)

GLASS redshifts Hoag et al. (2016);

^(b)

Balestra et al. (2016);

^(c)

Rodney et al., in prep.

^(d)

Grillo et al. (2015);

^(e)

Jauzac et al. (2014);

^(f)

Richard et al. (2014);

^(g)

Zitrin et al. (2013);

^(*)

Objects whose magnitude might be affected by source confusion.

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