adsabs/AstroCLIMB huggingface dataset:
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Wavelength calibration bias as a function of intrashutter source position, for both the prism (top) and medium gratings (bottom). δx is the spatial offset of the target with respect to the center of the microshutter, measured along the dispersion direction. For an unbiased wavelength solution, we would expect Δv = 0 at δx = 0 and δy = 0, and no correlation. The observed correlation with δx means that the correction we adopted for the intrashutter source position is insufficient (see Section 5 and P. Ferruit et al. 2022); δx increases toward bluer wavelengths. Neglecting intrashutter source position entirely would result in an even larger bias than what reported here.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Comparison of redshifts between the prism and the medium-resolution gratings. We find a redshift-independent offset Δ z = 0.0042 (blue line), consistent with B24; the shaded region is the standard deviation. The increased dispersion at low redshifts is expected from the strong dependence of the prism spectral resolution with wavelength. The black diamonds are the moving median; there is some evidence for a reduced bias around z < 1.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: The interface used to visually inspect NIRSpec data, showing GN-z11 (ID 5591 in Medium/JWST GOODS-N; P. A. Oesch et al. 2016; A. J. Bunker et al. 2023; R. Maiolino et al. 2024a). The console displays simultaneously the 1D spectrum and 2D S/N map. The user is able to move a set of bright spectral features to be used as reference (vertical dashed lines). The bottom row of console is the set of flags the user can assign.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Redshift vs. UV magnitude distribution of the sample, color coded by the equivalent width of [O III] λ5007 (empty symbols are galaxies with no detected [O III] λ5007). Magnitudes were calculated directly from the prism spectra, using aperture corrections estimated by comparing the prism magnitude to the 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩35 radius magnitude (CIRC5 in the catalogs) in the NIRCam filter nearest to rest-frame 1500 Å. [O III] λ5007 falls outside of the NIRSpec wavelength range at z ≳ 9.5.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Redshift distribution of the sample, color coded by the final redshift flag (Section 9). We note a drop in redshift distribution at zSpec ~ 7.5; this reflects a similar drop in the distribution of photometric redshifts of the targets selected for observation.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Redshift vs. magnitude distribution of the sample; NIRSpec deep spectroscopy can measure redshifts for targets fainter than 30 mag.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Summary of the VI; the left column shows targets for which a redshift could not be determined (flag 1). Galaxies with uncertain redshifts (center) and with secure redshifts (right) are split by the highest-confidence redshift flag, colored as labeled. Overall, the current success rate of JADES redshifts is 65%.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Wavelength solution bias Δv as a function of location on the MSA; the four rectangles are the four MSA quadrants Q1–Q4, with the location of the sample galaxies marked by small gray dots. The large dots represent galaxies with more than four emission lines detected at S/N > 5, for which we could calculate the velocity offset between lines observed at wavelengths of 1–2 μm and lines observed at 3–5.3 μm. Δv has been corrected empirically for the residual intrashutter wavelength bias (Section 9. 〈Δv〉 is the average of Δv inside each of the quadrants, illustrating a trend of increasing bias diagonally from Q3 to Q2.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Comparison of the prism emission-line fluxes and their uncertainties between DR1 and DR3: the top row compares the fluxes, the bottom row compares the uncertainties. We find a statistically significant correlation between the ratio of uncertainties and flux (panel (d)), indicating that our PPXF implementation tends to underestimate the line noise in the high-S/N regime, relative to DR1. The gray points in the bottom panel illustrate the effect of adding 1% relative uncertainties to the DR3 flux measurements.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Comparison of the Hβ flux measured from the prism between DR1 and DR3; the symbols are the same as in Figure 23. Below redshift z = 2, Hβ is blended with [O III] λλ4959, 5007 and is not reported in this figure. The Hβ flux ratio between DR3 and DR1 is 1.04, while for all emission lines the ratio is 1.003.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Comparison of the medium-resolution emission-line fluxes and their uncertainties between DR1 and DR3: the top row compares the fluxes, the bottom row compares the uncertainties. Fluxes are in excellent agreement, while we find the uncertainties to be smaller by 20%, on average.
Paper: Toward Higher-order Accuracy in Self-gravitating Hydrodynamics
Authors: Tomoyuki Hanawa, Patrick D. Mullen
Figure caption: The black line denotes the gravity as a function of the cell center position in the cells along the line of yj = zj = 0.05R for the polytrope of n = 1 with an envelope. The red line denotes the deviation from the cell average.
Paper: Toward Higher-order Accuracy in Self-gravitating Hydrodynamics
Authors: Tomoyuki Hanawa, Patrick D. Mullen
Figure caption: Same as Figure 10, but after the large density gradient correction. The red line denotes the deviation magnified by a factor of 50.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: A low-redshift quiescent galaxy, displaying a smooth, peaked light distribution and an evolved stellar population. Panel (a) shows a false-color NIRCam image, with the adopted filters in the bottom right corner. Panel (b) is the NIRSpec/MSA 2D S/N map of the prism spectrum; three shutters are indicated. Here and in all other 2D maps (Figures 15(b)–20(b)), negative S/N is caused by the nod-and-subtract strategy for removing the background. Panel (c) is the 1D, 5 pixel box-car extracted spectrum. Besides the strong 4000 Å break, several stellar and interstellar medium (ISM) absorption features are detected. Notice that the aperture correction applied in this data reduction is optimized for pointlike sources; extended galaxies like 200733 would require both a different aperture correction and a different background-subtraction strategy, to avoid self-subtraction. From W. M. Baker et al. (2024).
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: “Pablo’s Galaxy,” a UVJ-quiescent galaxy at z = 3 hosting an X-ray and mid-infrared (MIR) AGN and multiphase outflows. This system displays a rich set of stellar and ISM absorption lines (Mg II λλ2796, 2803 and Na I λλ5890, 5896, the latter tracing a fast neutral-gas outflow; F. D’Eugenio et al. 2024a). Emission lines trace both low-ionization gas, including [O II] λλ3726, 3729, [O I] λλ6300, 6363, [N II] λλ6548, 6583, and [S II] λλ6716, 6731, possibly due to shocked or stripped gas, as well as higher-ionization species ([Ne V] λλ3346, 3426). Note the flux-calibration offset between G140M (blue) and G235M (light blue: 10%) and G235M and G395M (blue; 7%). Like 200733 (Figure 14), Pablo’s Galaxy is fairly extended, meaning the standard aperture correction and background subtraction are not optimal. From J. Scholtz et al. (2024). All symbols are the same as Figure 14.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Example of a dust-reddened AGN host, with clear outflows (as seen in the broad component of forbidden [O III] λλ4959, 5007, [S II] λλ6716, 6731, and [S III] λλ9069, 9532), stellar continuum (there is evidence of a Balmer break), and high temperature lines (from the detection of several auroral lines, [O II] λλ7319–7332 and [S II] λλ10290–10373). The blue line in panel (c) is the (spliced) medium-resolution grating spectra (gaps are due to the gaps between the NIRSpec detectors). The black rectangles show details of the Hβ + [O III] λλ4959, 5007 and Hα + [N II] λλ6548, 6583 to [S II] λλ6716, 6731 emission-line regions. All other symbols are the same as Figure 14.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: One of the highest-redshift sources in this data release, 96216 (JADES-GS-z12-0; E. Curtis-Lake et al. 2023; B. E. Robertson et al. 2023; 2773; B24). This system shows the highest-redshift detection of metals to date (F. D’Eugenio et al. 2024b). All symbols and panels are the same as Figure 14.