FRESCO: An extended, massive, rapidly rotating galaxy at z=5.3
| Autor: | Nelson, Erica J., Brammer, Gabriel, Gimenez-Arteaga, Clara, Oesch, Pascal A., Ubler, Hannah, de Graaff, Anna, Matharu, Jasleen, Naidu, Rohan P., Shapley, Alice E., Whitaker, Katherine E., Wisnioski, Emily, Schreiber, Natascha M. Forster, Smit, Renske, van Dokkum, Pieter, Chisholm, John, Endsley, Ryan, Hartley, Abigail I., Gibson, Justus, Giovinazzo, Emma, Illingworth, Garth, Labbe, Ivo, Maseda, Michael V., Matthee, Jorryt, Paz, Alba Covelo, Price, Sedona H., Reddy, Naveen A., Shivaei, Irene, Weibel, Andrea, Wuyts, Stijn, Xiao, Mengyuan, Alberts, Stacey, Baker, William M., Bunker, Andrew J., Cameron, Alex J., Charlot, Stephane, Eisenstein, Daniel J., Ji, Zhiyuan, Johnson, Benjamin D., Jones, Gareth C., Maiolino, Roberto, Robertson, Brant, Sandles, Lester, Suess, Katherine A., Tacchella, Sandro, Williams, Christina C., Witstok, Joris |
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| Rok vydání: | 2023 |
| Předmět: | |
| Druh dokumentu: | Working Paper |
| Popis: | With the remarkable sensitivity and resolution of JWST in the infrared, measuring rest-optical kinematics of galaxies at $z>5$ has become possible for the first time. This study pilots a new method for measuring galaxy dynamics for highly multiplexed, unbiased samples by combining FRESCO NIRCam grism spectroscopy and JADES medium-band imaging. Here we present one of the first JWST kinematic measurements for a galaxy at $z>5$. We find a significant velocity gradient, which, if interpreted as rotation yields $V_{rot} = 240\pm50$km/s and we hence refer to this galaxy as Twister-z5. With a rest-frame optical effective radius of $r_e=2.25$kpc, the high rotation velocity in this galaxy is not due to a compact size as may be expected in the early universe but rather a high total mass, ${\rm log(M}_{dyn}/{\rm M}_\odot)=11.0\pm0.2$. This is a factor of roughly 4x higher than the stellar mass within the effective radius. We also observe that the radial H$\alpha$ equivalent width profile and the specific star formation rate map from resolved stellar population modeling is centrally depressed by a factor of $\sim1.5$ from the center to $r_e$. Combined with the morphology of the line-emitting gas in comparison to the continuum, this centrally suppressed star formation is consistent with a star-forming disk surrounding a bulge growing inside-out. While large, rapidly rotating disks are common to z~2, the existence of one after only 1Gyr of cosmic time, shown for the first time in ionized gas, adds to the growing evidence that some galaxies matured earlier than expected in the history of the universe. Comment: Fig. 3 shows the main result |
| Databáze: | arXiv |
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