Discovery and characterization of the highest-redshift barred spiral galaxy candidate at z=5.102, with bar length ~4.5 kpc, stellar mass 10^10.45 solar masses, SFR 144 solar masses per year, and evidence for AGN and interaction.
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- method Crucially, theσ LOS distributions for star-forming spaxels are very similar in field and cluster environ- ments. The median Hα σ LOS for star-forming re- gions is 27 km s −1 in PHANGS-MUSE and 30 km s −1 in MAUVE-MUSE, with narrow interquartile ranges (12 km s −1 and 6 km s −1, respectively) and 90% ranges 14 SF spaxels non-SF spaxels 0 1 2 3density PHANGS MUSE H LOS 40 km s 1 H LOS = [40, 80) km s 1 H LOS > 80 km s 1 SF spaxels non-SF spaxels PHANGS MUSE 1.0 0.5 0.0 0.5 1.0 dSF, NII [dex] 0 1 2
- method The presence of forbidden emission lines of neutral and singly ionized atoms is one of the criteria defining the FS CMa group [8]. The oxygen doublet [OI] λλ 6300, 6364 Å is always present. Especially important are lines of [SII] λλ 6716, 6731 Å and [NII] λλ 6548, 6583 Å that allow the usage of nebular diagnostics, e.g., Baldwin, Phillips & Terlevich (BPT) diagrams [9]. Forbidden emission lines are very narrow (FWHM ≈ 50 km s−1), symmetric, and sometimes double-peaked. They are used as tracers o
- background The right graph plots logarithm Himass vs. stellar mass in solar units. The light gray dots are galaxies in ALFALFA survey and contours represent the 100, 400, 800 number density levels within a 0.25x0.25 bin. T able 1.Basic information of our Seyfert galaxy sample. Galaxy RA [J2000] DEC [J2000]d[Mpc] logM ∗ [M⊙] SNR GMRT Observation Date (1) (2) (3) (4) (5) (6) (7) UGC 4503a 13h 35m 19s.24 +26 d 25m 29s.10 62.2 10.82 90.1 2024/08/24 UGC 6128a 11h 04m 02s.95 +28 d 02m 12s.30 24.1 9.94 81.9 2024/
- background emission) from ionized hydrogen in star-forming regions, while a few sources are likely dominated by synchrotron 4 T able 1.SF-Consistent Radio Sources with VLA-9 Detections FIRST (1993-2011; 5 ′′) VLASS (2017-2024; 2.′′5) VLA-9 (2014; 0.′′25) IDS 1.4 GHz σ1.4 GHz log(L1.4 GHz )S 3 GHz σ3 GHz log(L3 GHz )α S 9 GHz σ9 GHz log(L9 GHz ) Major Axis Point Source (1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) 7 0.73 0.09 20.6 1.18a 0.36 20.8 0.6(0.4) 172 20 19.9 158 F 11 2.37 0.15 20.9 1.85 0
- other Note-Each module name is listed only in the first relevant row, and all multi-line values are preserved as in the original table. Unlisted parameters are set to the default values. T able 4.NuSTAR Photometric Properties Obsid Observation Exposure Time Net Source Counts P B Start Date (ks) 3-8 keV 8-24 keV 3-24 keV 3-8 keV 8-24 keV 3-24 keV (1) (2) (3) (4) (5) (6) (7) (8) (9) 61001007002 2024-12-03 59.8<42.0 27.9 +16.9 −15.9 50.5+23.7 −22.4 0.031 0.009 0.001 61001007004 2024-12-07 46.2<21.4<13.3<
- baseline 7<z<2.0 7.5-8.0 -2.08±0.20 [22] - - - - 8.0-8.5 -2.00±0.07 [37] - - - - 8.5-9.0 -2.22±0.09 [23] - - - - 9.0-9.5 -2.29±0.11 [16] -2.57±0.14 [15] -2.75±0.23 [5] - - 9.5-10.0 -2.43±0.13 [11] -2.78±0.08 [31] -2.48±0.08 [37] - - 10.0-10.5 -2.49±0.14 [9] -2.91±0.09 [22] -2.59±0.08 [33] -3.29±0.29 [3] - 10.5-11.0 -2.50±0.14 [9] -3.12±0.12 [14] -2.79±0.09 [21] -2.78±0.06 [32] -3.09±0.20 [17] 11.0-11.5 -2.68±0.17[6] -2.93±0.09[22] -2.62±0.08 [39] -2.67±0.05 [55] -2.93±0.09 [43] 11.5-12.0 - -3.16±0.12 [13
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citing papers explorer
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A massive barred spiral galaxy at z = 5.102 discovered by JWST
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