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125 results on '"Willmer, Christopher N. A."'

1. Spectroscopic confirmation of two luminous galaxies at a redshift of 14

Author

Carniani, Stefano, Hainline, Kevin, D’Eugenio, Francesco, Eisenstein, Daniel J., Jakobsen, Peter, Witstok, Joris, Johnson, Benjamin D., Chevallard, Jacopo, Maiolino, Roberto, Helton, Jakob M., Willott, Chris, Robertson, Brant, Alberts, Stacey, Arribas, Santiago, Baker, William M., Bhatawdekar, Rachana, Boyett, Kristan, Bunker, Andrew J., Cameron, Alex J., Cargile, Phillip A., Charlot, Stéphane, Curti, Mirko, Curtis-Lake, Emma, Egami, Eiichi, Giardino, Giovanna, Isaak, Kate, Ji, Zhiyuan, Jones, Gareth C., Kumari, Nimisha, Maseda, Michael V., Parlanti, Eleonora, Pérez-González, Pablo G., Rawle, Tim, Rieke, George, Rieke, Marcia, Del Pino, Bruno Rodríguez, Saxena, Aayush, Scholtz, Jan, Smit, Renske, Sun, Fengwu, Tacchella, Sandro, Übler, Hannah, Venturi, Giacomo, Williams, Christina C., and Willmer, Christopher N. A.

Published
2024
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2. A small and vigorous black hole in the early Universe

Author

Maiolino, Roberto, Scholtz, Jan, Witstok, Joris, Carniani, Stefano, D’Eugenio, Francesco, de Graaff, Anna, Übler, Hannah, Tacchella, Sandro, Curtis-Lake, Emma, Arribas, Santiago, Bunker, Andrew, Charlot, Stéphane, Chevallard, Jacopo, Curti, Mirko, Looser, Tobias J., Maseda, Michael V., Rawle, Timothy D., Rodríguez del Pino, Bruno, Willott, Chris J., Egami, Eiichi, Eisenstein, Daniel J., Hainline, Kevin N., Robertson, Brant, Williams, Christina C., Willmer, Christopher N. A., Baker, William M., Boyett, Kristan, DeCoursey, Christa, Fabian, Andrew C., Helton, Jakob M., Ji, Zhiyuan, Jones, Gareth C., Kumari, Nimisha, Laporte, Nicolas, Nelson, Erica J., Perna, Michele, Sandles, Lester, Shivaei, Irene, and Sun, Fengwu

Published
2024
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3. Author Correction: A small and vigorous black hole in the early Universe

Author

Maiolino, Roberto, Scholtz, Jan, Witstok, Joris, Carniani, Stefano, D’Eugenio, Francesco, de Graaff, Anna, Übler, Hannah, Tacchella, Sandro, Curtis-Lake, Emma, Arribas, Santiago, Bunker, Andrew, Charlot, Stéphane, Chevallard, Jacopo, Curti, Mirko, Looser, Tobias J., Maseda, Michael V., Rawle, Timothy D., Rodríguez del Pino, Bruno, Willott, Chris J., Egami, Eiichi, Eisenstein, Daniel J., Hainline, Kevin N., Robertson, Brant, Williams, Christina C., Willmer, Christopher N. A., Baker, William M., Boyett, Kristan, DeCoursey, Christa, Fabian, Andrew C., Helton, Jakob M., Ji, Zhiyuan, Jones, Gareth C., Kumari, Nimisha, Laporte, Nicolas, Nelson, Erica J., Perna, Michele, Sandles, Lester, Shivaei, Irene, and Sun, Fengwu

Published
2024
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4. Carbonaceous dust grains seen in the first billion years of cosmic time

Author

Witstok, Joris, Shivaei, Irene, Smit, Renske, Maiolino, Roberto, Carniani, Stefano, Curtis-Lake, Emma, Ferruit, Pierre, Arribas, Santiago, Bunker, Andrew J., Cameron, Alex J., Charlot, Stephane, Chevallard, Jacopo, Curti, Mirko, de Graaff, Anna, D’Eugenio, Francesco, Giardino, Giovanna, Looser, Tobias J., Rawle, Tim, Rodríguez del Pino, Bruno, Willott, Chris, Alberts, Stacey, Baker, William M., Boyett, Kristan, Egami, Eiichi, Eisenstein, Daniel J., Endsley, Ryan, Hainline, Kevin N., Ji, Zhiyuan, Johnson, Benjamin D., Kumari, Nimisha, Lyu, Jianwei, Nelson, Erica, Perna, Michele, Rieke, Marcia, Robertson, Brant E., Sandles, Lester, Saxena, Aayush, Scholtz, Jan, Sun, Fengwu, Tacchella, Sandro, Williams, Christina C., and Willmer, Christopher N. A.

Published
2023
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5. Spectroscopic confirmation of four metal-poor galaxies at z = 10.3–13.2

Author

Curtis-Lake, Emma, Carniani, Stefano, Cameron, Alex, Charlot, Stephane, Jakobsen, Peter, Maiolino, Roberto, Bunker, Andrew, Witstok, Joris, Smit, Renske, Chevallard, Jacopo, Willott, Chris, Ferruit, Pierre, Arribas, Santiago, Bonaventura, Nina, Curti, Mirko, D’Eugenio, Francesco, Franx, Marijn, Giardino, Giovanna, Looser, Tobias J., Lützgendorf, Nora, Maseda, Michael V., Rawle, Tim, Rix, Hans-Walter, Rodríguez del Pino, Bruno, Übler, Hannah, Sirianni, Marco, Dressler, Alan, Egami, Eiichi, Eisenstein, Daniel J., Endsley, Ryan, Hainline, Kevin, Hausen, Ryan, Johnson, Benjamin D., Rieke, Marcia, Robertson, Brant, Shivaei, Irene, Stark, Daniel P., Tacchella, Sandro, Williams, Christina C., Willmer, Christopher N. A., Bhatawdekar, Rachana, Bowler, Rebecca, Boyett, Kristan, Chen, Zuyi, de Graaff, Anna, Helton, Jakob M., Hviding, Raphael E., Jones, Gareth C., Kumari, Nimisha, Lyu, Jianwei, Nelson, Erica, Perna, Michele, Sandles, Lester, Saxena, Aayush, Suess, Katherine A., Sun, Fengwu, Topping, Michael W., Wallace, Imaan E. B., and Whitler, Lily

Published
2023
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6. JWST's PEARLS: Mothra, a new kaiju star at z=2.091 extremely magnified by MACS0416, and implications for dark matter models

Author

Diego, J. M., Sun, Bangzheng, Yan, Haojing, Furtak, Lukas J., Zackrisson, Erik, Dai, Liang, Kelly, Patrick, Nonino, Mario, Adams, Nathan, Meena, Ashish K., Willner, S. P., Zitrin, Adi, Cohen, Seth H., Silva, Jordan C. J. D, Jansen, Rolf A., Summers, Jake, Windhorst, Rogier A., Coe, Dan, Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Koekemoer, Anton M., Marshall, Madeline A., Pirzkal, Nor, Robotham, Aaron, Rutkowski, Michael J., Ryan, Russell E., Tompkins, Scott, Willmer, Christopher N. A., and Bhatawdekar, Rachana

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the discovery of Mothra, an extremely magnified monster star, likely a binary system of two supergiant stars, in one of the strongly lensed galaxies behind the galaxy cluster MACS0416. The star is in a galaxy with spectroscopic redshift $z=2.091$ in a portion of the galaxy that is parsecs away from the cluster caustic. The binary star is observed only on the side of the critical curve with negative parity but has been detectable for at least eight years, implying the presence of a small lensing perturber. Microlenses alone cannot explain the earlier observations of this object made with the Hubble Space Telescope. A larger perturber with a mass of at least $10^4$\,\Msun\ offers a more satisfactory explanation. Based on the lack of perturbation on other nearby sources in the same arc, the maximum mass of the perturber is $M< 2.5\times10^6$\,\Msun, making it the smallest substructure constrained by lensing above redshift 0.3. The existence of this millilens is fully consistent with the expectations from the standard cold dark matter model. On the other hand, the existence of such small substructure in a cluster environment has implications for other dark matter models. In particular, warm dark matter models with particle masses below 8.7\,keV are excluded by our observations. Similarly, axion dark matter models are consistent with the observations only if the axion mass is in the range $0.5\times10^{-22}\, {\rm eV} < m_a < 5\times10^{-22}\, {\rm eV}$., 26 pages and 27 figures

Published
2023

7. EPOCHS VII: Discovery of high redshift ($6.5 < z < 12$) AGN candidates in JWST ERO and PEARLS data

Author

Juodžbalis, Ignas, Conselice, Christopher J., Singh, Maitrayee, Adams, Nathan, Ormerod, Katherine, Harvey, Thomas, Austin, Duncan, Volonteri, Marta, Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Windhorst, Rogier A., D'Silva, Jordan C. J., Koekemoer, Anton M., Coe, Dan, Driver, Simon P., Frye, Brenda, Grogin, Norman A., Marshall, Madeline A., Nonino, Mario, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Ortiz III, Rafael, Tompkins, Scott, Willmer, Christopher N. A., and Yan, Haojing

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present an analysis of a sample of robust high redshift galaxies selected photometrically from the `blank' fields of the Prime Extragalactic Areas for Reionization Science (PEARLS) survey and Early Release Observations (ERO) data of the James Webb Space Telescope (JWST) with the aim of selecting candidate high redshift active galactic nuclei (AGN). Sources were identified from the parent sample using a threefold selection procedure, which includes spectral energy distribution (SED) fitting to identify sources that are best fitted by AGN SED templates, a further selection based on the relative performance of AGN and non-AGN models, and finally morphological fitting to identify compact sources of emission, resulting in a purity-oriented procedure. Using this procedure, we identify a sample of nine AGN candidates at $6.5 < z < 12$, from which we constrain their physical properties as well as measure a lower bound on the AGN fraction in this redshift range of $5 \pm 1$\%. As this is an extreme lower limit due to our focus on purity and our SEDs being calibrated for unobscured Type 1 AGN, this demonstrates that AGN are perhaps quite common at this early epoch. The rest-frame UV colors of our candidate objects suggest that these systems are potentially candidate obese black hole galaxies (OBG), or AGN with very little galaxy component. We also investigate emission from our sample sources from fields overlapping with Chandra and VLA surveys, allowing us to place X-ray and 3 GHz radio detection limits on our candidates. Of note is a $z = 11.9$ candidate source exhibiting an abrupt morphological shift in the reddest band as compared to the bluer bands, indicating a potential merger or an unusually strong outflow., Comment: Submitted to MNRAS, 12 pages, 11 figures, typos corrected

Published
2023

8. Magellanic System Stars Identified in SMACS J0723.3-7327 James Webb Space Telescope Early Release Observations Images.

Author

Summers, Jake, Windhorst, Rogier A., Cohen, Seth H., Jansen, Rolf A., Carleton, Timothy, Kamieneski, Patrick S., Holwerda, Benne W., Conselice, Christopher J., Adams, Nathan J., Frye, Brenda L., Diego, Jose M., Willmer, Christopher N. A., Ortiz III, Rafael, Cheng, Cheng, Pigarelli, Alex, Robotham, Aaron, D'Silva, Jordan C. J., Tompkins, Scott, Driver, Simon P., and Yan, Haojing

Subjects
SPACE telescopes, LARGE magellanic cloud, DENSITY of stars, SPECTRAL energy distribution, STELLAR parallax, MAGELLANIC clouds
Abstract

We identify 71 distant stars in James Webb Space Telescope/NIRCam early release observations (ERO) images of the field of galaxy cluster SMACS J0723.3-7327 (SMACS 0723). Given the relatively small (∼10°) angular separation between SMACS 0723 and the Large Magellanic Cloud (LMC), it is likely that these stars are associated with the LMC outskirts or the Leading Arm. This is further bolstered by a spectral energy distribution (SED) analysis, which suggests an excess of stars at a physical distance of 40–100 kpc, consistent with being associated with or located behind the Magellanic system. In particular, we find that the overall surface density of stars brighter than 27.0 mag in the field of SMACS 0723 is ∼2.3 times that of stars in a blank field with similar Galactic latitude (the North Ecliptic Pole Time Domain Field), and that the density of stars in the SMACS 0723 field with SED-derived distances consistent with the Magellanic system is ∼6.1 times larger than that of the blank field. The candidate stars at these distances are consistent with a stellar population at the same distance modulus with [Fe/H] = −1.0 and an age of ∼5.0 Gyr. On the assumption that all of the 71 stars are associated with the LMC, then the stellar density of the LMC at the location of the SMACS 0723 field is ∼740 stars kpc−3, which helps trace the density of stars in the LMC outskirts. [ABSTRACT FROM AUTHOR]

Published
2023
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9. Are JWST/NIRCam Color Gradients in the Lensed z = 2.3 Dusty Star-forming Galaxy El Anzuelo Due to Central Dust Attenuation or Inside-out Galaxy Growth?

Author

Kamieneski, Patrick S., Frye, Brenda L., Pascale, Massimo, Cohen, Seth H., Windhorst, Rogier A., Jansen, Rolf A., Yun, Min S., Cheng, Cheng, Summers, Jake S., Carleton, Timothy, Harrington, Kevin C., Diego, Jose M., Yan, Haojing, Koekemoer, Anton M., Willmer, Christopher N. A., Petric, Andreea, Furtak, Lukas J., Foo, Nicholas, Conselice, Christopher J., and Coe, Dan

Subjects
STAR formation, GALACTIC redshift, SPECTRAL energy distribution, DUST, STELLAR populations, GALAXIES
Abstract

Gradients in the mass-to-light ratio of distant galaxies impede our ability to characterize their size and compactness. The long-wavelength filters of JWST's NIRCam offer a significant step forward. For galaxies at Cosmic Noon (z ∼ 2), this regime corresponds to the rest-frame near-infrared, which is less biased toward young stars and captures emission from the bulk of a galaxy's stellar population. We present an initial analysis of an extraordinary lensed dusty star-forming galaxy at z = 2.3 behind the El Gordo cluster (z = 0.87), named El Anzuelo ("The Fishhook") after its partial Einstein-ring morphology. The far-UV to near-IR spectral energy distribution suggests an intrinsic star formation rate of 81 − 2 + 7 M ⊙ yr − 1 and dust attenuation A V ≈ 1.6, in line with other DSFGs on the star-forming main sequence. We develop a parametric lens model to reconstruct the source-plane structure of dust imaged by the Atacama Large Millimeter/submillimeter Array, far-UV to optical light from Hubble, and near-IR imaging with 8 filters of JWST/NIRCam, as part of the Prime Extragalactic Areas for Reionization and Lensing Science program. The source-plane half-light radius is remarkably consistent from ∼1 to 4.5 μ m, despite a clear color gradient where the inferred galaxy center is redder than the outskirts. We interpret this to be the result of both a radially decreasing gradient in attenuation and substantial spatial offsets between UV- and IR-emitting components. A spatial decomposition of the SED reveals modestly suppressed star formation in the inner kiloparsec, which suggests that we are witnessing the early stages of inside-out quenching. [ABSTRACT FROM AUTHOR]

Published
2023
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10. Magellanic System Stars Identified in the SMACS J0723.3-7327 JWST ERO Images

Author

Summers, Jake, Windhorst, Rogier A., Cohen, Seth H., Jansen, Rolf A., Carleton, Timothy, Kamieneski, Patrick S., Holwerda, Benne W., Conselice, Christopher J., Adams, Nathan J., Frye, Brenda, Diego, Jose M., Willmer, Christopher N. A., Ortiz, Rafael, Cheng, Cheng, Pigarelli, Alex, Robotham, Aaron, D'Silva, Jordan C. J., Tompkins, Scott, Driver, Simon P., Yan, Haojing, Coe, Dan, Grogin, Norman, Koekemoer, Anton, Marshall, Madeline A., Pirzkal, Nor, and Ryan, Russell E.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

We identify 68 distant stars in JWST/NIRCam ERO images of the field of galaxy cluster SMACS J0723.3-7327 (SMACS 0723). Given the relatively small ($\sim$$10^{\circ}$) angular separation between SMACS 0723 and the Large Magellanic Cloud, it is likely that these stars are associated with the LMC outskirts or Leading Arm. This is further bolstered by a spectral energy distribution analysis, which suggests an excess of stars at a physical distance of $40-100$ kpc, consistent with being associated with or located behind the Magellanic system. In particular, we find that the overall surface density of stars brighter than 27.0 mag in the field of SMACS 0723 is $\sim$2.3 times that of stars in a blank field with similar galactic latitude (the North Ecliptic Pole Time Domain Field), and that the density of stars in the SMACS 0723 field with SED-derived distances consistent with the Magellanic system is $\sim$7.3 times larger than that of the blank field. The candidate stars at these distances are consistent with a stellar population at the same distance modulus with [Fe/H] $= -1.0$ and an age of $\sim$$5.0$ Gyr. On the assumption that all of the 68 stars are associated with the LMC, then the stellar density of the LMC at the location of the SMACS 0723 field is $\sim$$710$ stars kpc$^{-3}$, which helps trace the density of stars in the LMC outskirts., Submitted to ApJ, comments welcome

Published
2023

11. JADES NIRSpec Initial Data Release for the Hubble Ultra Deep Field: Redshifts and Line Fluxes of Distant Galaxies from the Deepest JWST Cycle 1 NIRSpec Multi-Object Spectroscopy

Author

Bunker, Andrew J., Cameron, Alex J., Curtis-Lake, Emma, Jakobsen, Peter, Carniani, Stefano, Curti, Mirko, Witstok, Joris, Maiolino, Roberto, D'Eugenio, Francesco, Looser, Tobias J., Willott, Chris, Bonaventura, Nina, Hainline, Kevin, Uebler, Hannah, Willmer, Christopher N. A., Saxena, Aayush, Smit, Renske, Alberts, Stacey, Arribas, Santiago, Baker, William M., Baum, Stefi, Bhatawdekar, Rachana, Bowler, Rebecca A. A., Boyett, Kristan, Charlot, Stephane, Chen, Zuyi, Chevallard, Jacopo, Circosta, Chiara, DeCoursey, Christa, de Graaff, Anna, Egami, Eiichi, Eisenstein, Daniel J., Endsley, Ryan, Ferruit, Pierre, Giardino, Giovanna, Hausen, Ryan, Helton, Jakob M., Hviding, Raphael E., Ji, Zhiyuan, Johnson, Benjamin D., Jones, Gareth C., Kumari, Nimisha, Laseter, Isaac, Luetzgendorf, Nora, Maseda, Michael V., Nelson, Erica, Parlanti, Eleonora, Perna, Michele, Rawle, Tim, Rix, Hans-Walter, Rieke, Marcia, Robertson, Brant, Del Pino, Bruno Rodriguez, Sandles, Lester, Scholtz, Jan, Sharpe, Katherine, Skarbinski, Maya, Stark, Daniel P., Sun, Fengwu, Tacchella, Sandro, Topping, Michael W., Villanueva, Natalia C., Wallace, Imaan E. B., Williams, Christina C., and Woodrum, Charity

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

We describe the NIRSpec component of the JWST Deep Extragalactic Survey (JADES), and provide deep spectroscopy of 253 sources targeted with the NIRSpec micro-shutter assembly in the Hubble Ultra Deep Field and surrounding GOODS-South. The multi-object spectra presented here are the deepest so far obtained with JWST, amounting to up to 28 hours in the low-dispersion ($R\sim 30-300$) prism, and up to 7 hours in each of the three medium-resolution $R\approx 1000$ gratings and one high-dispersion grating, G395H ($R\approx2700$). Our low-dispersion and medium-dispersion spectra cover the wavelength range $0.6-5.3μ$m. We describe the selection of the spectroscopic targets, the strategy for the allocation of targets to micro-shutters, and the design of the observations. We present the public release of the reduced 2D and 1D spectra, and a description of the reduction and calibration process. We measure spectroscopic redshifts for 178 of the objects targeted extending up to $z=13.2$. We present a catalog of all emission lines detected at $S/N>5$, and our redshift determinations for the targets. Combined with the first JADES NIRCam data release, these public JADES spectroscopic and imaging datasets provide a new foundation for discoveries of the infrared universe by the worldwide scientific community., Submitted to A&A. Data products available from https://archive.stsci.edu/hlsp/jades

Published
2023

12. Overview of the JWST Advanced Deep Extragalactic Survey (JADES)

Author

Eisenstein, Daniel J., Willott, Chris, Alberts, Stacey, Arribas, Santiago, Bonaventura, Nina, Bunker, Andrew J., Cameron, Alex J., Carniani, Stefano, Charlot, Stephane, Curtis-Lake, Emma, D'Eugenio, Francesco, Endsley, Ryan, Ferruit, Pierre, Giardino, Giovanna, Hainline, Kevin, Hausen, Ryan, Jakobsen, Peter, Johnson, Benjamin D., Maiolino, Roberto, Rieke, Marcia, Rieke, George, Rix, Hans-Walter, Robertson, Brant, Stark, Daniel P., Tacchella, Sandro, Williams, Christina C., Willmer, Christopher N. A., Baker, William M., Baum, Stefi, Bhatawdekar, Rachana, Boyett, Kristan, Chen, Zuyi, Chevallard, Jacopo, Circosta, Chiara, Curti, Mirko, Danhaive, A. Lola, DeCoursey, Christa, de Graaff, Anna, Dressler, Alan, Egami, Eiichi, Helton, Jakob M., Hviding, Raphael E., Ji, Zhiyuan, Jones, Gareth C., Kumari, Nimisha, Lützgendorf, Nora, Laseter, Isaac, Looser, Tobias J., Lyu, Jianwei, Maseda, Michael V., Nelson, Erica, Parlanti, Eleonora, Perna, Michele, Puskás, Dávid, Rawle, Tim, Del Pino, Bruno Rodríguez, Sandles, Lester, Saxena, Aayush, Scholtz, Jan, Sharpe, Katherine, Shivaei, Irene, Silcock, Maddie S., Simmonds, Charlotte, Skarbinski, Maya, Smit, Renske, Stone, Meredith, Suess, Katherine A., Sun, Fengwu, Tang, Mengtao, Topping, Michael W., Übler, Hannah, Villanueva, Natalia C., Wallace, Imaan E. B., Whitler, Lily, Witstok, Joris, and Woodrum, Charity

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

We present an overview of the James Webb Space Telescope (JWST) Advanced Deep Extragalactic Survey (JADES), an ambitious program of infrared imaging and spectroscopy in the GOODS-S and GOODS-N deep fields, designed to study galaxy evolution from high redshift to cosmic noon. JADES uses about 770 hours of Cycle 1 guaranteed time largely from the Near-Infrared Camera (NIRCam) and Near-Infrared Spectrograph (NIRSpec) instrument teams. In GOODS-S, in and around the Hubble Ultra Deep Field and Chandra Deep Field South, JADES produces a deep imaging region of ~45 arcmin$^2$ with an average of 130 hrs of exposure time spread over 9 NIRCam filters. This is extended at medium depth in GOODS-S and GOODS-N with NIRCam imaging of ~175 arcmin$^2$ with an average exposure time of 20 hrs spread over 8-10 filters. In both fields, we conduct extensive NIRSpec multi-object spectroscopy, including 2 deep pointings of 55 hrs exposure time, 14 medium pointings of ~12 hrs, and 15 shallower pointings of ~4 hrs, targeting over 5000 HST and JWST-detected faint sources with 5 low, medium, and high-resolution dispersers covering 0.6-5.3 microns. Finally, JADES extends redward via coordinated parallels with the JWST Mid-Infrared Instrument (MIRI), featuring ~9 arcmin$^2$ with 43 hours of exposure at 7.7 microns and twice that area with 2-6.5 hours of exposure at 12.8 microns For nearly 30 years, the GOODS-S and GOODS-N fields have been developed as the premier deep fields on the sky; JADES is now providing a compelling start on the JWST legacy in these fields., 33 pages, submitted to ApJ Supplement. The JADES Collaboration web site is at https://jades-survey.github.io, and the initial data release is available at https://archive.stsci.edu/hlsp/jades with a viewer at http://jades.idies.jhu.edu

Published
2023

13. The Cosmos in its Infancy: JADES Galaxy Candidates at z > 8 in GOODS-S and GOODS-N

Author

Hainline, Kevin N., Johnson, Benjamin D., Robertson, Brant, Tacchella, Sandro, Helton, Jakob M., Sun, Fengwu, Eisenstein, Daniel J., Simmonds, Charlotte, Topping, Michael W., Whitler, Lily, Willmer, Christopher N. A., Rieke, Marcia, Suess, Katherine A., Hviding, Raphael E., Cameron, Alex J., Alberts, Stacey, Baker, William M., Bhatawdekar, Rachana, Boyett, Kristan, Bunker, Andrew J., Carniani, Stefano, Charlot, Stephane, Chen, Zuyi, Curti, Mirko, Curtis-Lake, Emma, D'Eugenio, Francesco, Egami, Eiichi, Endsley, Ryan, Hausen, Ryan, Ji, Zhiyuan, Looser, Tobias J., Lyu, Jianwei, Maiolino, Roberto, Nelson, Erica, Puskas, David, Rawle, Tim, Sandles, Lester, Saxena, Aayush, Smit, Renske, Stark, Daniel P., Williams, Christina C., Willott, Chris, and Witstok, Joris

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a catalog of 717 candidate galaxies at $z > 8$ selected from 125 square arcminutes of NIRCam imaging as part of the JWST Advanced Deep Extragalactic Survey (JADES). We combine the full JADES imaging dataset with data from the JEMS and FRESCO JWST surveys along with extremely deep existing observations from HST/ACS for a final filter set that includes fifteen JWST/NIRCam filters and five HST/ACS filters. The high-redshift galaxy candidates were selected from their estimated photometric redshifts calculated using a template fitting approach, followed by visual inspection from seven independent reviewers. We explore these candidates in detail, highlighting interesting resolved or extended sources, sources with very red long-wavelength slopes, and our highest redshift candidates, which extend to $z_{phot} = 18$. We also investigate potential contamination by stellar objects, and do not find strong evidence from SED fitting that these faint high-redshift galaxy candidates are low-mass stars. Over 93\% of the sources are newly identified from our deep JADES imaging, including 31 new galaxy candidates at $z_{phot} > 12$. Using 42 sources in our sample with measured spectroscopic redshifts from NIRSpec and FRESCO, we find excellent agreement to our photometric redshift estimates, with no catastrophic outliers and an average difference of $\langle \Delta z = z_{phot}- z_{spec} \rangle= 0.26$. These sources comprise one of the most robust samples for probing the early buildup of galaxies within the first few hundred million years of the Universe's history., Comment: v2: 40 pages, 18 figures, submitted to AAS Journals, online data catalog (JADES Deep only) found at https://doi.org/10.5281/zenodo.8092529

Published
2023

14. JADES + JEMS: A Detailed Look at the Buildup of Central Stellar Cores and Suppression of Star Formation in Galaxies at Redshifts 3 < z < 4.5

Author

Ji, Zhiyuan, Williams, Christina C., Tacchella, Sandro, Suess, Katherine A., Baker, William M., Alberts, Stacey, Bunker, Andrew J., Johnson, Benjamin D., Robertson, Brant, Sun, Fengwu, Eisenstein, Daniel J., Rieke, Marcia, Maseda, Michael V., Hainline, Kevin, Hausen, Ryan, Rieke, George, Willmer, Christopher N. A., Egami, Eiichi, Shivaei, Irene, Carniani, Stefano, Charlot, Stephane, Chevallard, Jacopo, Curtis-Lake, Emma, Looser, Tobias J., Maiolino, Roberto, Willott, Chris, Chen, Zuyi, Helton, Jakob M., Lyu, Jianwei, Nelson, Erica, Bhatawdekar, Rachana, Boyett, Kristan, and Sandles, Lester

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a spatially resolved study of stellar populations in 6 galaxies with stellar masses $M_*\sim10^{10}M_\odot$ at $z\sim3.7$ using 14-filter JWST/NIRCam imaging from the JADES and JEMS surveys. The 6 galaxies are visually selected to have clumpy substructures with distinct colors over rest-frame $3600-4100$\r{A}, including a bright dominant stellar core that is close to their stellar-light centroids. With 23-filter photometry from HST to JWST, we measure the stellar-population properties of individual structural components via SED fitting using Prospector. We find that the central stellar cores are $\gtrsim2$ times more massive than the Toomre mass, indicating they may not form via in-situ fragmentation. The stellar cores have stellar ages of $0.4-0.7$ Gyr that are similar to the timescale of clump inward migration due to dynamical friction, suggesting that they likely instead formed through the coalescence of giant stellar clumps. While they have not yet quenched, the 6 galaxies are below the star-forming main sequence by $0.2-0.7$ dex. Within each galaxy, we find that the specific star formation rate is lower in the central stellar core, and the stellar-mass surface density of the core is already similar to quenched galaxies of the same masses and redshifts. Meanwhile, the stellar ages of the cores are either comparable to or younger than the extended, smooth parts of the galaxies. Our findings are consistent with model predictions of the gas-rich compaction scenario for the buildup of galaxies' central regions at high redshifts. We are likely witnessing the coeval formation of dense central cores, along with the onset of galaxy-wide quenching at $z>3$., Comment: 32 pages, 16 figures, submitted to ApJ. Comments are welcome

Published
2023

15. EPOCHS Paper II: The Ultraviolet Luminosity Function from $7.5<z<13.5$ using 110 square arcminutes of deep, blank-field data from the PEARLS Survey and Public Science Programmes

Author

Adams, Nathan J., Conselice, Christopher J., Austin, Duncan, Harvey, Thomas, Ferreira, Leonardo, Trussler, James, Juodzbalis, Ignas, Li, Qiong, Windhorst, Rogier, Cohen, Seth H., Jansen, Rolf, Summers, Jake, Tompkins, Scott, Driver, Simon P., Robotham, Aaron, D'Silva, Jordan C. J., Yan, Haojing, Coe, Dan, Frye, Brenda, Grogin, Norman A., Koekemoer, Anton M., Marshall, Madeline A., Pirzkal, Nor, Ryan, Jr., Russell E., Maksym, W. Peter, Rutkowski, Michael J., Willmer, Christopher N. A., Hammel, Heidi B., Nonino, Mario, Bhatawdekar, Rachana, Wilkins, Stephen M., Willner, Steven P., Bradley, Larry D., Broadhurst, Tom, Cheng, Cheng, Dole, Herve, Hathi, Nimish P., and Zitrin, Adi

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present an analysis of the ultraviolet luminosity function (UV LF) and star formation rate density of distant galaxies ($7.5 < z < 13.5$) in the `blank' fields of the Prime Extragalactic Areas for Reionization Science (PEARLS) survey combined with Early Release Science (ERS) data from the CEERS, GLASS and NGDEEP surveys/fields. We use a combination of SED fitting tools and quality cuts to obtain a reliable selection and characterisation of high-redshift ($z>6.5$) galaxies from a consistently processed set of deep, near-infrared imaging. Within an area of 110 arcmin$^{2}$, we identify 214 candidate galaxies at redshifts $z>6.5$ and we use this sample to study the ultraviolet luminosity function (UV LF) in four redshift bins between $7.5, Comment: 28 Pages, 4 Tables, 9 Figures, Submitted to ApJ

Published
2023

16. Are JWST/NIRCam color gradients in the lensed z=2.3 dusty star-forming galaxy El Anzuelo due to central dust attenuation or inside-out galaxy growth?

Author

Kamieneski, Patrick S., Frye, Brenda L., Pascale, Massimo, Cohen, Seth H., Windhorst, Rogier A., Jansen, Rolf A., Yun, Min S., Cheng, Cheng, Summers, Jake S., Carleton, Timothy, Harrington, Kevin C., Diego, Jose M., Yan, Haojing, Koekemoer, Anton M., Willmer, Christopher N. A., Petric, Andreea, Furtak, Lukas J., Foo, Nicholas, Conselice, Christopher J., Coe, Dan, Driver, Simon P., Grogin, Norman A., Marshall, Madeline A., Pirzkal, Nor, Robotham, Aaron S. G., Ryan Jr., Russell E., and Tompkins, Scott

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Gradients in the mass-to-light ratio of distant galaxies impede our ability to characterize their size and compactness. The long-wavelength filters of $JWST$'s NIRCam offer a significant step forward. For galaxies at Cosmic Noon ($z\sim2$), this regime corresponds to the rest-frame near-infrared, which is less biased towards young stars and captures emission from the bulk of a galaxy's stellar population. We present an initial analysis of an extraordinary lensed dusty star-forming galaxy (DSFG) at $z=2.3$ behind the $El~Gordo$ cluster ($z=0.87$), named $El~Anzuelo$ ("The Fishhook") after its partial Einstein-ring morphology. The FUV-NIR SED suggests an intrinsic star formation rate of $81^{+7}_{-2}~M_\odot~{\rm yr}^{-1}$ and dust attenuation $A_V\approx 1.6$, in line with other DSFGs on the star-forming main sequence. We develop a parametric lens model to reconstruct the source-plane structure of dust imaged by the Atacama Large Millimeter/submillimeter Array, far-UV to optical light from $Hubble$, and near-IR imaging with 8 filters of $JWST$/NIRCam, as part of the Prime Extragalactic Areas for Reionization and Lensing Science (PEARLS) program. The source-plane half-light radius is remarkably consistent from $\sim 1-4.5~\mu$m, despite a clear color gradient where the inferred galaxy center is redder than the outskirts. We interpret this to be the result of both a radially-decreasing gradient in attenuation and substantial spatial offsets between UV- and IR-emitting components. A spatial decomposition of the SED reveals modestly suppressed star formation in the inner kiloparsec, which suggests that we are witnessing the early stages of inside-out quenching., Comment: 29 pages, 11 figures, 5 tables. Accepted for publication in ApJ

Published
2023

17. JADES: Discovery of extremely high equivalent width Lyman-alpha emission from a faint galaxy within an ionized bubble at z=7.3

Author

Saxena, Aayush, Robertson, Brant E., Bunker, Andrew J., Endsley, Ryan, Cameron, Alex J., Charlot, Stephane, Simmonds, Charlotte, Tacchella, Sandro, Witstok, Joris, Willott, Chris, Carniani, Stefano, Curtis-Lake, Emma, Ferruit, Pierre, Jakobsen, Peter, Arribas, Santiago, Chevallard, Jacopo, Curti, Mirko, D'Eugenio, Francesco, De Graaff, Anna, Jones, Gareth C., Looser, Tobias J., Maseda, Michael V., Rawle, Tim, Rix, Hans-Walter, Del Pino, Bruno Rodríguez, Smit, Renske, Übler, Hannah, Eisenstein, Daniel J., Hainline, Kevin, Hausen, Ryan, Johnson, Benjamin D., Rieke, Marcia, Williams, Christina C., Willmer, Christopher N. A., Baker, William M., Bhatawdekar, Rachana, Bowler, Rebecca, Boyett, Kristan, Chen, Zuyi, Egami, Eiichi, Ji, Zhiyuan, Nelson, Erica, Perna, Michele, Sandles, Lester, Scholtz, Jan, and Shivaei, Irene

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the discovery of a remarkable Ly$\alpha$ emitting galaxy at $z=7.278$, JADES-GS+53.16746-27.7720 (shortened to JADES-GS-z7-LA), with EW$_0$(Ly$\alpha$) $\approx400 \pm 90$A and UV magnitude $-16.7$. The spectroscopic redshift is confirmed via rest-frame optical lines [O II], H$\beta$ and [O III] in its JWST/NIRSpec Micro-Shutter Assembly (MSA) spectrum. The Ly$\alpha$ line is detected in both lower resolution ($R\sim100$) PRISM as well as medium resolution ($R\sim1000$) G140M grating spectra. The Ly$\alpha$ FWHM in the grating is $\approx360$ km s$^{-1}$ and the line peaks within $120$ km s$^{-1}$ of the systemic redshift, indicative of very little neutral gas or dust within the galaxy. We estimate the Ly$\alpha$ escape fraction to be $\sim100\%$. JADES-GS-z7-LA has a [O III]/[O II] ratio (O32) of $8.8 \pm 1.1$ and ([O III]+[O II])/H$\beta$ ratio (R23) of $9.6\pm2.2$, consistent with low metallicity and high ionization parameters. Deep NIRCam imaging also revealed a close companion source (separated by $0.23''$), which exhibits similar photometry to that of JADES-GS-z7-LA, with a photometric excess in the F410M NIRCam image consistent with [O III]+H$\beta$ emission at the same redshift. The spectral energy distribution of JADES-GS-z7-LA indicates a `bursty' star-formation history, with a low stellar mass of $10^{7.15}$ M$_\odot$. The only explanation of the high EW Ly$\alpha$ emission seen in JADES-GS-z7-LA is if it resides in an ionized bubble with radius $\gtrsim 3$ pMpc. Owing to the faint nature of JADES-GS-z7-LA, we show that it is incapable of single-handedly ionizing a bubble large enough. Therefore, we suggest that JADES-GS-z7-LA (and possibly the companion source) may be a part of a larger overdensity, presenting direct evidence of overlapping ionized bubbles at $z>7$, allowing us to study the process of reionization across both small and large scales., Comment: 12 pages, 7 figures, submitted to Astronomy & Astrophysics, comments welcome!

Published
2023

18. JADES NIRSpec Spectroscopy of GN-z11: Lyman-$\alpha$ emission and possible enhanced nitrogen abundance in a $z=10.60$ luminous galaxy

Author

Bunker, Andrew J., Saxena, Aayush, Cameron, Alex J., Willott, Chris J., Curtis-Lake, Emma, Jakobsen, Peter, Carniani, Stefano, Smit, Renske, Maiolino, Roberto, Witstok, Joris, Curti, Mirko, D'Eugenio, Francesco, Jones, Gareth C., Ferruit, Pierre, Arribas, Santiago, Charlot, Stephane, Chevallard, Jacopo, Giardino, Giovanna, de Graaff, Anna, Looser, Tobias J., Luetzgendorf, Nora, Maseda, Michael V., Rawle, Tim, Rix, Hans-Walter, Del Pino, Bruno Rodriguez, Alberts, Stacey, Egami, Eiichi, Eisenstein, Daniel J., Endsley, Ryan, Hainline, Kevin, Hausen, Ryan, Johnson, Benjamin D., Rieke, George, Rieke, Marcia, Robertson, Brant E., Shivaei, Irene, Stark, Daniel P., Sun, Fengwu, Tacchella, Sandro, Tang, Mengtao, Williams, Christina C., Willmer, Christopher N. A., Baker, William M., Baum, Stefi, Bhatawdekar, Rachana, Bowler, Rebecca, Boyett, Kristan, Chen, Zuyi, Circosta, Chiara, Helton, Jakob M., Ji, Zhiyuan, Lyu, Jianwei, Nelson, Erica, Parlanti, Eleonora, Perna, Michele, Sandles, Lester, Scholtz, Jan, Suess, Katherine A., Topping, Michael W., Uebler, Hannah, Wallace, Imaan E. B., and Whitler, Lily

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present JADES JWST/NIRSpec spectroscopy of GN-z11, the most luminous candidate $z>10$ Lyman break galaxy in the GOODS-North field with $M_{UV}=-21.5$. We derive a redshift of $z=10.603$ (lower than previous determinations) based on multiple emission lines in our low and medium resolution spectra over $0.8-5.3 \mu$m. We significantly detect the continuum and measure a blue rest-UV spectral slope of $\beta=-2.4$. Remarkably, we see spatially-extended Lyman-$\alpha$ in emission (despite the highly-neutral IGM expected at this early epoch), offset 555 km s$^{-1}$ redward of the systemic redshift. From our measurements of collisionally-excited lines of both low- and high-ionization (including [O II]$\lambda3727$, [Ne III]$\lambda 3869$ and C III]$\lambda1909$) we infer a high ionization parameter ($\log U\sim -2$). We detect the rarely-seen N IV]$\lambda1486$ and N III]$\lambda1748$ lines in both our low and medium resolution spectra, with other high ionization lines seen in the low resolution spectrum such as He II (blended with O III]) and C IV (with a possible P-Cygni profile). Based on the observed rest-UV line ratios, we cannot conclusively rule out photoionization from AGN, although the high C III]/He II and N III]/He II ratios are compatible with a star-formation explanation. If the observed emission lines are powered by star formation, then the strong N III]$\lambda1748$ observed may imply an unusually high $N/O$ abundance. Balmer emission lines (H$\gamma$, H$\delta$) are also detected, and if powered by star formation rather than an AGN we infer a star formation rate of $\sim 20-30 M_{\odot} yr^{-1}$ (depending on the IMF) and low dust attenuation. Our NIRSpec spectroscopy confirms that GN-z11 is a remarkable galaxy with extreme properties seen 430 Myr after the Big Bang., Comment: Accepted for publication in Astronomy & Astrophysics, 17 pages, 12 figures. Line fluxes updated

Published
2023

19. JADES Imaging of GN-z11: Revealing the Morphology and Environment of a Luminous Galaxy 430 Myr After the Big Bang

Author

Tacchella, Sandro, Eisenstein, Daniel J., Hainline, Kevin, Johnson, Benjamin D., Baker, William M., Helton, Jakob M., Robertson, Brant, Suess, Katherine A., Chen, Zuyi, Nelson, Erica, Puskás, Dávid, Sun, Fengwu, Alberts, Stacey, Egami, Eiichi, Hausen, Ryan, Rieke, George, Rieke, Marcia, Shivaei, Irene, Williams, Christina C., Willmer, Christopher N. A., Bunker, Andrew, Cameron, Alex J., Carniani, Stefano, Charlot, Stephane, Curti, Mirko, Curtis-Lake, Emma, Looser, Tobias J., Maiolino, Roberto, Maseda, Michael V., Rawle, Tim, Rix, Hans-Walter, Smit, Renske, Übler, Hannah, Willott, Chris, Witstok, Joris, Baum, Stefi, Bhatawdekar, Rachana, Boyett, Kristan, Danhaive, A. Lola, de Graaff, Anna, Endsley, Ryan, Ji, Zhiyuan, Lyu, Jianwei, Sandles, Lester, Saxena, Aayush, Scholtz, Jan, Topping, Michael W., and Whitler, Lily

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies
Abstract

We present JWST NIRCam 9-band near-infrared imaging of the luminous $z=10.6$ galaxy GN-z11 from the JWST Advanced Deep Extragalactic Survey (JADES) of the GOODS-N field. We find a spectral energy distribution (SED) entirely consistent with the expected form of a high-redshift galaxy: a clear blue continuum from 1.5 to 4 microns with a complete dropout in F115W. The core of GN-z11 is extremely compact in JWST imaging. We analyze the image with a two-component model, using a point source and a S\'{e}rsic profile that fits to a half-light radius of 200 pc and an index $n=0.9$. We find a low-surface brightness haze about $0.4''$ to the northeast of the galaxy, which is most likely a foreground object but might be a more extended component of GN-z11. At a spectroscopic redshift of 10.60 (Bunker et al. 2023), the comparison of the NIRCam F410M and F444W images spans the Balmer jump. From population synthesis modeling, here assuming no light from an active galactic nucleus, we reproduce the SED of GN-z11, finding a stellar mass of $\sim$$10^{9}~M_{\odot}$, a star-formation rate of $\sim$$20~M_{\odot}~\mathrm{yr}^{-1}$ and a young stellar age of $\sim$$20~\mathrm{Myr}$. As massive galaxies at high redshift are likely to be highly clustered, we search for faint neighbors of GN-z11, finding 9 galaxies out to $\sim$5 comoving Mpc transverse with photometric redshifts consistent with $z=10.6$, and a 10$^{\rm th}$ more tentative dropout only $3''$ away. This is consistent with GN-z11 being hosted by a massive dark-matter halo ($\approx8\times10^{10}~M_{\odot}$), though lower halo masses cannot be ruled out., Comment: 18 pages, 8 figures, accepted for publication in ApJ

Published
2023

20. JEMS: A deep medium-band imaging survey in the Hubble Ultra-Deep Field with JWST NIRCam & NIRISS

Author

Williams, Christina C., Tacchella, Sandro, Maseda, Michael V., Robertson, Brant E., Johnson, Benjamin D., Willott, Chris J., Eisenstein, Daniel J., Willmer, Christopher N. A., Ji, Zhiyuan, Hainline, Kevin N., Helton, Jakob M., Alberts, Stacey, Baum, Stefi, Bhatawdekar, Rachana, Boyett, Kristan, Bunker, Andrew J., Carniani, Stefano, Charlot, Stephane, Chevallard, Jacopo, Curtis-Lake, Emma, de Graaf, Anna, Egami, Eiichi, Franx, Marijn, Kumari, Nimisha, Maiolino, Roberto, Nelson, Erica J., Rieke, Marcia J., Sandles, Lester, Shivaei, Irene, Simmonds, Charlotte, Smit, Renske, Suess, Katherine A., Sun, Fengwu, Ubler, Hannah, and Witstok, Joris

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present JEMS (JWST Extragalactic Medium-band Survey), the first public medium-band imaging survey carried out using JWST/NIRCam and NIRISS. These observations use $\sim2\mu$m and $\sim4\mu$m medium-band filters (NIRCam F182M, F210M, F430M, F460M, F480M; and NIRISS F430M & F480M in parallel) over 15.6 square arcminutes in the Hubble Ultra Deep Field (UDF), thereby building on the deepest multi-wavelength public datasets available anywhere on the sky. We describe our science goals, survey design, NIRCam and NIRISS image reduction methods, and describe our first data release of the science-ready mosaics. Our chosen filters create a JWST imaging survey in the UDF that enables novel analysis of a range of spectral features potentially across the redshift range of $0.31$ magnitude) across redshifts $1.5, Comment: Submitted to AAS Journals, comments welcome. First data release including science-ready mosaics after peer-review

Published
2023

21. The James Webb Space Telescope Mission

Author

Gardner, Jonathan P., Mather, John C., Abbott, Randy, Abell, James S., Abernathy, Mark, Abney, Faith E., Abraham, John G., Abraham, Roberto, Abul-Huda, Yasin M., Acton, Scott, Adams, Cynthia K., Adams, Evan, Adler, David S., Adriaensen, Maarten, Aguilar, Jonathan Albert, Ahmed, Mansoor, Ahmed, Nasif S., Ahmed, Tanjira, Albat, Rüdeger, Albert, Loïc, Alberts, Stacey, Aldridge, David, Allen, Mary Marsha, Allen, Shaune S., Altenburg, Martin, Altunc, Serhat, Alvarez, Jose Lorenzo, Álvarez-Márquez, Javier, de Oliveira, Catarina Alves, Ambrose, Leslie L., Anandakrishnan, Satya M., Andersen, Gregory C., Anderson, Harry James, Anderson, Jay, Anderson, Kristen, Anderson, Sara M., Aprea, Julio, Archer, Benita J., Arenberg, Jonathan W., Argyriou, Ioannis, Arribas, Santiago, Artigau, Étienne, Arvai, Amanda Rose, Atcheson, Paul, Atkinson, Charles B., Averbukh, Jesse, Aymergen, Cagatay, Bacinski, John J., Baggett, Wayne E., Bagnasco, Giorgio, Baker, Lynn L., Balzano, Vicki Ann, Banks, Kimberly A., Baran, David A., Barker, Elizabeth A., Barrett, Larry K., Barringer, Bruce O., Barto, Allison, Bast, William, Baudoz, Pierre, Baum, Stefi, Beatty, Thomas G., Beaulieu, Mathilde, Bechtold, Kathryn, Beck, Tracy, Beddard, Megan M., Beichman, Charles, Bellagama, Larry, Bely, Pierre, Berger, Timothy W., Bergeron, Louis E., Darveau-Bernier, Antoine, Bertch, Maria D., Beskow, Charlotte, Betz, Laura E., Biagetti, Carl P., Birkmann, Stephan, Bjorklund, Kurt F., Blackwood, James D., Blazek, Ronald Paul, Blossfeld, Stephen, Bluth, Marcel, Boccaletti, Anthony, Boegner Jr., Martin E., Bohlin, Ralph C., Boia, John Joseph, Böker, Torsten, Bonaventura, N., Bond, Nicholas A., Bosley, Kari Ann, Boucarut, Rene A., Bouchet, Patrice, Bouwman, Jeroen, Bower, Gary, Bowers, Ariel S., Bowers, Charles W., Boyce, Leslye A., Boyer, Christine T., Boyer, Martha L., Boyer, Michael, Boyer, Robert, Bradley, Larry D., Brady, Gregory R., Brandl, Bernhard R., Brannen, Judith L., Breda, David, Bremmer, Harold G., Brennan, David, Bresnahan, Pamela A., Bright, Stacey N., Broiles, Brian J., Bromenschenkel, Asa, Brooks, Brian H., Brooks, Keira J., Brown, Bob, Brown, Bruce, Brown, Thomas M., Bruce, Barry W., Bryson, Jonathan G., Bujanda, Edwin D., Bullock, Blake M., Bunker, A. J., Bureo, Rafael, Burt, Irving J., Bush, James Aaron, Bushouse, Howard A., Bussman, Marie C., Cabaud, Olivier, Cale, Steven, Calhoon, Charles D., Calvani, Humberto, Canipe, Alicia M., Caputo, Francis M., Cara, Mihai, Carey, Larkin, Case, Michael Eli, Cesari, Thaddeus, Cetorelli, Lee D., Chance, Don R., Chandler, Lynn, Chaney, Dave, Chapman, George N., Charlot, S., Chayer, Pierre, Cheezum, Jeffrey I., Chen, Bin, Chen, Christine H., Cherinka, Brian, Chichester, Sarah C., Chilton, Zachary S., Chittiraibalan, Dharini, Clampin, Mark, Clark, Charles R., Clark, Kerry W., Clark, Stephanie M., Claybrooks, Edward E., Cleveland, Keith A., Cohen, Andrew L., Cohen, Lester M., Colón, Knicole D., Coleman, Benee L., Colina, Luis, Comber, Brian J., Comeau, Thomas M., Comer, Thomas, Reis, Alain Conde, Connolly, Dennis C., Conroy, Kyle E., Contos, Adam R., Contreras, James, Cook, Neil J., Cooper, James L., Cooper, Rachel Aviva, Correia, Michael F., Correnti, Matteo, Cossou, Christophe, Costanza, Brian F., Coulais, Alain, Cox, Colin R., Coyle, Ray T., Cracraft, Misty M., Noriega-Crespo, Alberto, Crew, Keith A., Curtis, Gary J., Cusveller, Bianca, Maciel, Cleyciane Da Costa, Dailey, Christopher T., Daugeron, Frédéric, Davidson, Greg S., Davies, James E., Davis, Katherine Anne, Davis, Michael S., Day, Ratna, de Chambure, Daniel, de Jong, Pauline, De Marchi, Guido, Dean, Bruce H., Decker, John E., Delisa, Amy S., Dell, Lawrence C., Dellagatta, Gail, Dembinska, Franciszka, Demosthenes, Sandor, Dencheva, Nadezhda M., Deneu, Philippe, DePriest, William W., Deschenes, Jeremy, Dethienne, Nathalie, Detre, Örs Hunor, Diaz, Rosa Izela, Dicken, Daniel, DiFelice, Audrey S., Dillman, Matthew, Disharoon, Maureen O., van Dishoeck, Ewine F., Dixon, William V., Doggett, Jesse B., Dominguez, Keisha L., Donaldson, Thomas S., Doria-Warner, Cristina M., Santos, Tony Dos, Doty, Heather, Douglas Jr., Robert E., Doyon, René, Dressler, Alan, Driggers, Jennifer, Driggers, Phillip A., Dunn, Jamie L., DuPrie, Kimberly C., Dupuis, Jean, Durning, John, Dutta, Sanghamitra B., Earl, Nicholas M., Eccleston, Paul, Ecobichon, Pascal, Egami, Eiichi, Ehrenwinkler, Ralf, Eisenhamer, Jonathan D., Eisenhower, Michael, Eisenstein, Daniel J., Hamel, Zaky El, Elie, Michelle L., Elliott, James, Elliott, Kyle Wesley, Engesser, Michael, Espinoza, Néstor, Etienne, Odessa, Etxaluze, Mireya, Evans, Leah, Fabreguettes, Luce, Falcolini, Massimo, Falini, Patrick R., Fatig, Curtis, Feeney, Matthew, Feinberg, Lee D., Fels, Raymond, Ferdous, Nazma, Ferguson, Henry C., Ferrarese, Laura, Ferreira, Marie-Héléne, Ferruit, Pierre, Ferry, Malcolm, Filippazzo, Joseph Charles, Firre, Daniel, Fix, Mees, Flagey, Nicolas, Flanagan, Kathryn A., Fleming, Scott W., Florian, Michael, Flynn, James R., Foiadelli, Luca, Fontaine, Mark R., Fontanella, Erin Marie, Forshay, Peter Randolph, Fortner, Elizabeth A., Fox, Ori D., Framarini, Alexandro P., Francisco, John I., Franck, Randy, Franx, Marijn, Franz, David E., Friedman, Scott D., Friend, Katheryn E., Frost, James R., Fu, Henry, Fullerton, Alexander W., Gaillard, Lionel, Galkin, Sergey, Gallagher, Ben, Galyer, Anthony D., Marín, Macarena García, Gardner, Lisa E., Garland, Dennis, Garrett, Bruce Albert, Gasman, Danny, Gáspár, András, Gastaud, René, Gaudreau, Daniel, Gauthier, Peter Timothy, Geers, Vincent, Geithner, Paul H., Gennaro, Mario, Gerber, John, Gereau, John C., Giampaoli, Robert, Giardino, Giovanna, Gibbons, Paul C., Gilbert, Karolina, Gilman, Larry, Girard, Julien H., Giuliano, Mark E., Gkountis, Konstantinos, Glasse, Alistair, Glassmire, Kirk Zachary, Glauser, Adrian Michael, Glazer, Stuart D., Goldberg, Joshua, Golimowski, David A., Gonzaga, Shireen P., Gordon, Karl D., Gordon, Shawn J., Goudfrooij, Paul, Gough, Michael J., Graham, Adrian J., Grau, Christopher M., Green, Joel David, Greene, Gretchen R., Greene, Thomas P., Greenfield, Perry E., Greenhouse, Matthew A., Greve, Thomas R., Greville, Edgar M., Grimaldi, Stefano, Groe, Frank E., Groebner, Andrew, Grumm, David M., Grundy, Timothy, Güdel, Manuel, Guillard, Pierre, Guldalian, John, Gunn, Christopher A., Gurule, Anthony, Gutman, Irvin Meyer, Guy, Paul D., Guyot, Benjamin, Hack, Warren J., Haderlein, Peter, Hagan, James B., Hagedorn, Andria, Hainline, Kevin, Haley, Craig, Hami, Maryam, Hamilton, Forrest Clifford, Hammann, Jeffrey, Hammel, Heidi B., Hanley, Christopher J., Hansen, Carl August, Hardy, Bruce, Harnisch, Bernd, Harr, Michael Hunter, Harris, Pamela, Hart, Jessica Ann, Hartig, George F., Hasan, Hashima, Hashim, Kathleen Marie, Hashimoto, Ryan, Haskins, Sujee J., Hawkins, Robert Edward, Hayden, Brian, Hayden, William L., Healy, Mike, Hecht, Karen, Heeg, Vince J., Hejal, Reem, Helm, Kristopher A., Hengemihle, Nicholas J., Henning, Thomas, Henry, Alaina, Henry, Ronald L., Henshaw, Katherine, Hernandez, Scarlin, Herrington, Donald C., Heske, Astrid, Hesman, Brigette Emily, Hickey, David L., Hilbert, Bryan N., Hines, Dean C., Hinz, Michael R., Hirsch, Michael, Hitcho, Robert S., Hodapp, Klaus, Hodge, Philip E., Hoffman, Melissa, Holfeltz, Sherie T., Holler, Bryan Jason, Hoppa, Jennifer Rose, Horner, Scott, Howard, Joseph M., Howard, Richard J., Huber, Jean M., Hunkeler, Joseph S., Hunter, Alexander, Hunter, David Gavin, Hurd, Spencer W., Hurst, Brendan J., Hutchings, John B., Hylan, Jason E., Ignat, Luminita Ilinca, Illingworth, Garth, Irish, Sandra M., Isaacs III, John C., Jackson Jr., Wallace C., Jaffe, Daniel T., Jahic, Jasmin, Jahromi, Amir, Jakobsen, Peter, James, Bryan, James, John C., James, LeAndrea Rae, Jamieson, William Brian, Jandra, Raymond D., Jayawardhana, Ray, Jedrzejewski, Robert, Jeffers, Basil S., Jensen, Peter, Joanne, Egges, Johns, Alan T., Johnson, Carl A., Johnson, Eric L., Johnson, Patricia, Johnson, Phillip Stephen, Johnson, Thomas K., Johnson, Timothy W., Johnstone, Doug, Jollet, Delphine, Jones, Danny P., Jones, Gregory S., Jones, Olivia C., Jones, Ronald A., Jones, Vicki, Jordan, Ian J., Jordan, Margaret E., Jue, Reginald, Jurkowski, Mark H., Justis, Grant, Justtanont, Kay, Kaleida, Catherine C., Kalirai, Jason S., Kalmanson, Phillip Cabrales, Kaltenegger, Lisa, Kammerer, Jens, Kan, Samuel K., Kanarek, Graham Childs, Kao, Shaw-Hong, Karakla, Diane M., Karl, Hermann, Kassin, Susan A., Kauffman, David D., Kavanagh, Patrick, Kelley, Leigh L., Kelly, Douglas M., Kendrew, Sarah, Kennedy, Herbert V., Kenny, Deborah A., Keski-Kuha, Ritva A., Keyes, Charles D., Khan, Ali, Kidwell, Richard C., Kimble, Randy A., King, James S., King, Richard C., Kinzel, Wayne M., Kirk, Jeffrey R., Kirkpatrick, Marc E., Klaassen, Pamela, Klingemann, Lana, Klintworth, Paul U., Knapp, Bryan Adam, Knight, Scott, Knollenberg, Perry J., Knutsen, Daniel Mark, Koehler, Robert, Koekemoer, Anton M., Kofler, Earl T., Kontson, Vicki L., Kovacs, Aiden Rose, Kozhurina-Platais, Vera, Krause, Oliver, Kriss, Gerard A., Krist, John, Kristoffersen, Monica R., Krogel, Claudia, Krueger, Anthony P., Kulp, Bernard A., Kumari, Nimisha, Kwan, Sandy W., Kyprianou, Mark, Labador, Aurora Gadiano, Labiano, Álvaro, Lafrenière, David, Lagage, Pierre-Olivier, Laidler, Victoria G., Laine, Benoit, Laird, Simon, Lajoie, Charles-Philippe, Lallo, Matthew D., Lam, May Yen, LaMassa, Stephanie Marie, Lambros, Scott D., Lampenfield, Richard Joseph, Lander, Matthew Ed, Langston, James Hutton, Larson, Kirsten, Larson, Melora, LaVerghetta, Robert Joseph, Law, David R., Lawrence, Jon F., Lee, David W., Lee, Janice, Lee, Yat-Ning Paul, Leisenring, Jarron, Leveille, Michael Dunlap, Levenson, Nancy A., Levi, Joshua S., Levine, Marie B., Lewis, Dan, Lewis, Jake, Lewis, Nikole, Libralato, Mattia, Lidon, Norbert, Liebrecht, Paula Louisa, Lightsey, Paul, Lilly, Simon, Lim, Frederick C., Lim, Pey Lian, Ling, Sai-Kwong, Link, Lisa J., Link, Miranda Nicole, Lipinski, Jamie L., Liu, XiaoLi, Lo, Amy S., Lobmeyer, Lynette, Logue, Ryan M., Long, Chris A., Long, Douglas R., Long, Ilana D., Long, Knox S., López-Caniego, Marcos, Lotz, Jennifer M., Love-Pruitt, Jennifer M., Lubskiy, Michael, Luers, Edward B., Luetgens, Robert A., Luevano, Annetta J., Lui, Sarah Marie G. Flores, Lund III, James M., Lundquist, Ray A., Lunine, Jonathan, Lützgendorf, Nora, Lynch, Richard J., MacDonald, Alex J., MacDonald, Kenneth, Macias, Matthew J., Macklis, Keith I., Maghami, Peiman, Maharaja, Rishabh Y., Maiolino, Roberto, Makrygiannis, Konstantinos G., Malla, Sunita Giri, Malumuth, Eliot M., Manjavacas, Elena, Marini, Andrea, Marrione, Amanda, Marston, Anthony, Martel, André R, Martin, Didier, Martin, Peter G., Martinez, Kristin L., Maschmann, Marc, Masci, Gregory L., Masetti, Margaret E., Maszkiewicz, Michael, Matthews, Gary, Matuskey, Jacob E., McBrayer, Glen A., McCarthy, Donald W., McCaughrean, Mark J., McClare, Leslie A., McClare, Michael D., McCloskey, John C., McClurg, Taylore D., McCoy, Martin, McElwain, Michael W., McGregor, Roy D., McGuffey, Douglas B., McKay, Andrew G., McKenzie, William K., McLean, Brian, McMaster, Matthew, McNeil, Warren, De Meester, Wim, Mehalick, Kimberly L., Meixner, Margaret, Meléndez, Marcio, Menzel, Michael P., Menzel, Michael T., Merz, Matthew, Mesterharm, David D., Meyer, Michael R., Meyett, Michele L., Meza, Luis E., Midwinter, Calvin, Milam, Stefanie N., Miller, Jay Todd, Miller, William C., Miskey, Cherie L., Misselt, Karl, Mitchell, Eileen P., Mohan, Martin, Montoya, Emily E., Moran, Michael J., Morishita, Takahiro, Moro-Martín, Amaya, Morrison, Debra L., Morrison, Jane, Morse, Ernie C., Moschos, Michael, Moseley, S. H., Mosier, Gary E., Mosner, Peter, Mountain, Matt, Muckenthaler, Jason S., Mueller, Donald G., Mueller, Migo, Muhiem, Daniella, Mühlmann, Prisca, Mullally, Susan Elizabeth, Mullen, Stephanie M., Munger, Alan J, Murphy, Jess, Murray, Katherine T., Muzerolle, James C., Mycroft, Matthew, Myers, Andrew, Myers, Carey R., Myers, Fred Richard R., Myers, Richard, Myrick, Kaila, Nagle IV, Adrian F., Nayak, Omnarayani, Naylor, Bret, Neff, Susan G., Nelan, Edmund P., Nella, John, Nguyen, Duy Tuong, Nguyen, Michael N., Nickson, Bryony, Nidhiry, John Joseph, Niedner, Malcolm B., Nieto-Santisteban, Maria, Nikolov, Nikolay K., Nishisaka, Mary Ann, Nota, Antonella, O'Mara, Robyn C., Oboryshko, Michael, O'Brien, Marcus B., Ochs, William R., Offenberg, Joel D., Ogle, Patrick Michael, Ohl, Raymond G., Olmsted, Joseph Hamden, Osborne, Shannon Barbara, O'Shaughnessy, Brian Patrick, Östlin, Göran, O'Sullivan, Brian, Otor, O. Justin, Ottens, Richard, Ouellette, Nathalie N. -Q., Outlaw, Daria J., Owens, Beverly A., Pacifici, Camilla, Page, James Christophe, Paranilam, James G., Park, Sang, Parrish, Keith A., Paschal, Laura, Patapis, Polychronis, Patel, Jignasha, Patrick, Keith, Pattishall Jr., Robert A., Paul, Douglas William, Paul, Shirley J., Pauly, Tyler Andrew, Pavlovsky, Cheryl M., Peña-Guerrero, Maria, Pedder, Andrew H., Peek, Matthew Weldon, Pelham, Patricia A., Penanen, Konstantin, Perriello, Beth A., Perrin, Marshall D., Perrine, Richard F., Perrygo, Chuck, Peslier, Muriel, Petach, Michael, Peterson, Karla A., Pfarr, Tom, Pierson, James M., Pietraszkiewicz, Martin, Pilchen, Guy, Pipher, Judy L., Pirzkal, Norbert, Pitman, Joseph T., Player, Danielle M., Plesha, Rachel, Plitzke, Anja, Pohner, John A., Poletis, Karyn Konstantin, Pollizzi, Joseph A., Polster, Ethan, Pontius, James T., Pontoppidan, Klaus, Porges, Susana C., Potter, Gregg D., Prescott, Stephen, Proffitt, Charles R., Pueyo, Laurent, Neira, Irma Aracely Quispe, Radich, Armando, Rager, Reiko T., Rameau, Julien, Ramey, Deborah D., Alarcon, Rafael Ramos, Rampini, Riccardo, Rapp, Robert, Rashford, Robert A., Rauscher, Bernard J., Ravindranath, Swara, Rawle, Timothy, Rawlings, Tynika N., Ray, Tom, Regan, Michael W., Rehm, Brian, Rehm, Kenneth D., Reid, Neill, Reis, Carl A., Renk, Florian, Reoch, Tom B., Ressler, Michael, Rest, Armin W., Reynolds, Paul J., Richon, Joel G., Richon, Karen V., Ridgaway, Michael, Riedel, Adric Richard, Rieke, George H., Rieke, Marcia, Rifelli, Richard E., Rigby, Jane R., Riggs, Catherine S., Ringel, Nancy J., Ritchie, Christine E., Rix, Hans-Walter, Robberto, Massimo, Robinson, Michael S., Robinson, Orion, Rock, Frank W., Rodriguez, David R., del Pino, Bruno Rodríguez, Roellig, Thomas, Rohrbach, Scott O., Roman, Anthony J., Romelfanger, Frederick J., Romo Jr., Felipe P., Rosales, Jose J., Rose, Perry, Roteliuk, Anthony F., Roth, Marc N., Rothwell, Braden Quinn, Rouzaud, Sylvain, Rowe, Jason, Rowlands, Neil, Roy, Arpita, Royer, Pierre, Rui, Chunlei, Rumler, Peter, Rumpl, William, Russ, Melissa L., Ryan, Michael B., Ryan, Richard M., Saad, Karl, Sabata, Modhumita, Sabatino, Rick, Sabbi, Elena, Sabelhaus, Phillip A., Sabia, Stephen, Sahu, Kailash C., Saif, Babak N., Salvignol, Jean-Christophe, Samara-Ratna, Piyal, Samuelson, Bridget S., Sanders, Felicia A., Sappington, Bradley, Sargent, B. A., Sauer, Arne, Savadkin, Bruce J., Sawicki, Marcin, Schappell, Tina M., Scheffer, Caroline, Scheithauer, Silvia, Scherer, Ron, Schiff, Conrad, Schlawin, Everett, Schmeitzky, Olivier, Schmitz, Tyler S., Schmude, Donald J., Schneider, Analyn, Schreiber, Jürgen, Schroeven-Deceuninck, Hilde, Schultz, John J., Schwab, Ryan, Schwartz, Curtis H., Scoccimarro, Dario, Scott, John F., Scott, Michelle B., Seaton, Bonita L., Seely, Bruce S., Seery, Bernard, Seidleck, Mark, Sembach, Kenneth, Shanahan, Clare Elizabeth, Shaughnessy, Bryan, Shaw, Richard A., Shay, Christopher Michael, Sheehan, Even, Sheth, Kartik, Shih, Hsin-Yi, Shivaei, Irene, Siegel, Noah, Sienkiewicz, Matthew G., Simmons, Debra D., Simon, Bernard P., Sirianni, Marco, Sivaramakrishnan, Anand, Slade, Jeffrey E., Sloan, G. C., Slocum, Christine E., Slowinski, Steven E., Smith, Corbett T., Smith, Eric P., Smith, Erin C., Smith, Koby, Smith, Robert, Smith, Stephanie J., Smolik, John L., Soderblom, David R., Sohn, Sangmo Tony, Sokol, Jeff, Sonneborn, George, Sontag, Christopher D., Sooy, Peter R., Soummer, Remi, Southwood, Dana M., Spain, Kay, Sparmo, Joseph, Speer, David T., Spencer, Richard, Sprofera, Joseph D., Stallcup, Scott S., Stanley, Marcia K., Stansberry, John A., Stark, Christopher C., Starr, Carl W., Stassi, Diane Y., Steck, Jane A., Steeley, Christine D., Stephens, Matthew A., Stephenson, Ralph J., Stewart, Alphonso C., Stiavelli, Massimo, Stockman Jr., Hervey, Strada, Paolo, Straughn, Amber N., Streetman, Scott, Strickland, David Kendal, Strobele, Jingping F., Stuhlinger, Martin, Stys, Jeffrey Edward, Such, Miguel, Sukhatme, Kalyani, Sullivan, Joseph F., Sullivan, Pamela C., Sumner, Sandra M., Sun, Fengwu, Sunnquist, Benjamin Dale, Swade, Daryl Allen, Swam, Michael S., Swenton, Diane F., Swoish, Robby A., Litten, Oi In Tam, Tamas, Laszlo, Tao, Andrew, Taylor, David K., Taylor, Joanna M., Plate, Maurice te, Van Tea, Mason, Teague, Kelly K., Telfer, Randal C., Temim, Tea, Texter, Scott C., Thatte, Deepashri G., Thompson, Christopher Lee, Thompson, Linda M., Thomson, Shaun R., Thronson, Harley, Tierney, C. M., Tikkanen, Tuomo, Tinnin, Lee, Tippet, William Thomas, Todd, Connor William, Tran, Hien D., Trauger, John, Trejo, Edwin Gregorio, Truong, Justin Hoang Vinh, Tsukamoto, Christine L., Tufail, Yasir, Tumlinson, Jason, Tustain, Samuel, Tyra, Harrison, Ubeda, Leonardo, Underwood, Kelli, Uzzo, Michael A., Vaclavik, Steven, Valenduc, Frida, Valenti, Jeff A., Van Campen, Julie, van de Wetering, Inge, Van Der Marel, Roeland P., van Haarlem, Remy, Vandenbussche, Bart, Vanterpool, Dona D., Vernoy, Michael R., Costas, Maria Begoña Vila, Volk, Kevin, Voorzaat, Piet, Voyton, Mark F., Vydra, Ekaterina, Waddy, Darryl J., Waelkens, Christoffel, Wahlgren, Glenn Michael, Walker Jr., Frederick E., Wander, Michel, Warfield, Christine K., Warner, Gerald, Wasiak, Francis C., Wasiak, Matthew F., Wehner, James, Weiler, Kevin R., Weilert, Mark, Weiss, Stanley B., Wells, Martyn, Welty, Alan D., Wheate, Lauren, Wheeler, Thomas P., White, Christy L., Whitehouse, Paul, Whiteleather, Jennifer Margaret, Whitman, William Russell, Williams, Christina C., Willmer, Christopher N. A., Willott, Chris J., Willoughby, Scott P., Wilson, Andrew, Wilson, Debra, Wilson, Donna V., Windhorst, Rogier, Wislowski, Emily Christine, Wolfe, David J., Wolfe, Michael A., Wolff, Schuyler, Wondel, Amancio, Woo, Cindy, Woods, Robert T., Worden, Elaine, Workman, William, Wright, Gillian S., Wu, Carl, Wu, Chi-Rai, Wun, Dakin D., Wymer, Kristen B., Yadetie, Thomas, Yan, Isabelle C., Yang, Keith C., Yates, Kayla L., Yeager, Christopher R., Yerger, Ethan John, Young, Erick T., Young, Gary, Yu, Gene, Yu, Susan, Zak, Dean S., Zeidler, Peter, Zepp, Robert, Zhou, Julia, Zincke, Christian A., Zonak, Stephanie, and Zondag, Elisabeth

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Twenty-six years ago a small committee report, building on earlier studies, expounded a compelling and poetic vision for the future of astronomy, calling for an infrared-optimized space telescope with an aperture of at least $4m$. With the support of their governments in the US, Europe, and Canada, 20,000 people realized that vision as the $6.5m$ James Webb Space Telescope. A generation of astronomers will celebrate their accomplishments for the life of the mission, potentially as long as 20 years, and beyond. This report and the scientific discoveries that follow are extended thank-you notes to the 20,000 team members. The telescope is working perfectly, with much better image quality than expected. In this and accompanying papers, we give a brief history, describe the observatory, outline its objectives and current observing program, and discuss the inventions and people who made it possible. We cite detailed reports on the design and the measured performance on orbit., Comment: Accepted by PASP for the special issue on The James Webb Space Telescope Overview, 29 pages, 4 figures

Published
2023

22. New $z > 7$ Lyman-alpha Emitters in EGS: Evidence of an Extended Ionized Structure at $z \sim 7.7$

Author

Jung, Intae, Finkelstein, Steven L., Larson, Rebecca L., Hutchison, Taylor A., Straughn, Amber N., Bagley, Micaela B., Castellano, Marco, Cleri, Nikko J., Cooper, M. C., Dickinson, Mark, Ferguson, Henry C., Holwerda, Benne W., Kartaltepe, Jeyhan S., Kim, Seonwoo, Koekemoer, Anton M., Papovich, Casey, Park, Hyunbae, Pentericci, Laura, Perez-Gonzalez, Pablo G., Song, Mimi, Tacchella, Sandro, Weiner, Benjamin J., Willmer, Christopher N. A., and Zavala, Jorge A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We perform a ground-based near-infrared spectroscopic survey using the Keck/MOSFIRE spectrograph to target Ly$\alpha$ emission at $7.0$4$\sigma$ level in eight $z>7$ galaxies, which include additional members of the known $z\sim7.7$ Ly$\alpha$-emitter (LAE) cluster (Tilvi et al. 2020). With the addition of these newly-discovered $z\sim7.7$ LAEs, this is currently the largest measured LAE cluster at $z>7$. The unusually-high Ly$\alpha$ detection rate at $z\sim7.7$ in this field suggests significantly stronger Ly$\alpha$ emission from the clustered LAEs than from the rest of our targets. We estimate the ionized bubble sizes around these LAEs and conclude that the LAEs are clustered within an extended ionized structure created by overlapping ionized bubbles which allow the easier escape of Ly$\alpha$ from galaxies. It is remarkable that the brightest object in the cluster has the lowest measured redshift of the Ly$\alpha$ line, being placed in front of the other LAEs in the line-of-sight direction. This suggests that we are witnessing the enhanced IGM transmission of Ly$\alpha$ from galaxies on the rear side of an ionized area. This could be a consequence of Ly$\alpha$ radiative transfer: Ly$\alpha$ close to the central velocity is substantially scattered by the IGM while Ly$\alpha$ from the rear-side galaxies is significantly redshifted to where it has a clear path., Comment: Submitted to ApJ (17 pages, 8 figures, 4 tables)

Published
2022

23. First Sample of H$\alpha$+[O III] $\lambda$5007 Line Emitters at $z > 6$ Through JWST/NIRCam Slitless Spectroscopy: Physical Properties and Line Luminosity Functions

Author

Sun, Fengwu, Egami, Eiichi, Pirzkal, Nor, Rieke, Marcia, Baum, Stefi, Boyer, Martha, Boyett, Kristan, Bunker, Andrew J., Cameron, Alex J., Curti, Mirko, Eisenstein, Daniel J., Gennaro, Mario, Greene, Thomas P., Jaffe, Daniel, Kelly, Doug, Koekemoer, Anton M., Kumari, Nimisha, Maiolino, Roberto, Maseda, Michael, Perna, Michele, Rest, Armin, Robertson, Brant E., Schlawin, Everett, Smit, Renske, Stansberry, John, Sunnquist, Ben, Tacchella, Sandro, Williams, Christina C., and Willmer, Christopher N. A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a sample of four emission-line galaxies at $z=6.11-6.35$ that were serendipitously discovered using the commissioning data for the JWST/NIRCam wide-field slitless spectroscopy (WFSS) mode. One of them (at $z=6.11$) has been reported previously while the others are new discoveries. These sources are selected by the secure detections of both [O III] $\lambda$5007 and H$\alpha$ lines with other fainter lines tentatively detected in some cases (e.g., [O II] $\lambda$3727, [O III] $\lambda$4959). In the [O III]/H$\beta$ - [N II]/H$\alpha$ Baldwin-Phillips-Terlevich diagram, these galaxies occupy the same parameter space as that of $z\sim2$ star-forming galaxies, indicating that they have been enriched rapidly to sub-solar metallicities ($\sim$0.4 $Z_{\odot}$), similar to galaxies with comparable stellar masses at much lower redshifts. The detection of strong H$\alpha$ lines suggests a higher ionizing photon production efficiency within galaxies in the early Universe. We find brightening of the [O III] $\lambda$5007 line luminosity function (LF) from $z=3$ to 6, and weak or no redshift evolution of the H$\alpha$ line LF from $z=2$ to 6. Both LFs are under-predicted at $z\sim6$ by a factor of $\sim$10 in certain cosmological simulations. This further indicates a global Ly$\alpha$ photon escape fraction of 7-10% at $z\sim6$, slightly lower than previous estimates through the comparison of the UV-derived star-formation rate density and Ly$\alpha$ luminosity density. Our sample recovers $66^{+128}_{-44}$% of $z=6.0-6.6$ galaxies in the survey volume with stellar masses greater than $5\times10^8$ $M_{\odot}$, suggesting the ubiquity of strong H$\alpha$ and [O III] line emitters in the Epoch of Reionization, which will be further uncovered in the era of JWST., Comment: 26 pages, 11 figures, accepted for publication in ApJ on May 11, 2023

Published
2022

24. CEERS Epoch 1 NIRCam Imaging: Reduction Methods and Simulations Enabling Early JWST Science Results.

Author

Bagley, Micaela B., Finkelstein, Steven L., Koekemoer, Anton M., Ferguson, Henry C., Haro, Pablo Arrabal, Dickinson, Mark, Kartaltepe, Jeyhan S., Papovich, Casey, Pérez-González, Pablo G., Pirzkal, Nor, Somerville, Rachel S., Willmer, Christopher N. A., Yang, Guang, Aaron Yung, L. Y., Fontana, Adriano, Grazian, Andrea, Grogin, Norman A., Hirschmann, Michaela, Kewley, Lisa J., and Kirkpatrick, Allison

Published
2023
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25. Performance of NIRCam on JWST in Flight.

Author

Rieke, Marcia J., Kelly, Douglas M., Misselt, Karl, Stansberry, John, Boyer, Martha, Beatty, Thomas, Egami, Eiichi, Florian, Michael, Greene, Thomas P., Hainline, Kevin, Leisenring, Jarron, Roellig, Thomas, Schlawin, Everett, Sun, Fengwu, Tinnin, Lee, Williams, Christina C., Willmer, Christopher N. A., Wilson, Debra, Clark, Charles R., and Rohrbach, Scott

Subjects
SPACE telescopes, INFRARED cameras, CAMERAS, ASTRONOMERS
Abstract

The Near Infrared Camera for the James Webb Space Telescope (JWST) is delivering the imagery that astronomers have hoped for ever since JWST was proposed back in the 1990s. In the Commissioning Period that extended from right after launch to early 2022 July, NIRCam has been subjected to a number of performance tests and operational checks. The camera is exceeding prelaunch expectations in virtually all areas, with very few surprises discovered in flight. NIRCam also delivered the imagery needed by the Wavefront Sensing Team for use in aligning the telescope mirror segments. [ABSTRACT FROM AUTHOR]

Published
2023
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26. JWST's PEARLS: Bright 1.5–2.0 μ m Dropouts in the Spitzer/IRAC Dark Field.

Author

Yan, Haojing, Cohen, Seth H., Windhorst, Rogier A., Jansen, Rolf A., Ma, Zhiyuan, Beacom, John F., Ling, Chenxiaoji, Cheng, Cheng, Huang, Jia-Sheng, Grogin, Norman A., Willner, S. P., Yun, Min, Hammel, Heidi B., Milam, Stefanie N., Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Marshall, Madeline A., Koekemoer, Anton, and Willmer, Christopher N. A.

Published
2023
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29. First Peek with JWST/NIRCam Wide-field Slitless Spectroscopy: Serendipitous Discovery of a Strong [O iii ]/H α Emitter at z = 6.11.

Author

Sun, Fengwu, Egami, Eiichi, Pirzkal, Nor, Rieke, Marcia, Boyer, Martha, Correnti, Matteo, Gennaro, Mario, Girard, Julien, Greene, Thomas P., Kelly, Doug, Koekemoer, Anton M., Leisenring, Jarron, Misselt, Karl, Nikolov, Nikolay, Roellig, Thomas L., Stansberry, John, Williams, Christina C., and Willmer, Christopher N. A.

Published
2022
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30. Searching for Low-redshift Faint Galaxies with MMT/Hectospec.

Author

Cheng, Cheng, Huang, Jia-Sheng, Willmer, Christopher N. A., Zhang, Hong-Xin, Ashby, Matthew L. N., Xu, Hai, Sawicki, Marcin, Arnouts, Stephane, Gwyn, Stephen, Desprez, Guilllaume, Coupon, Jean, Golob, Anneya, Liang, Piaoran, Cao, Tianwen, Shi, Yaru, Jin, Gaoxiang, He, Chuan, Wu, Shumei, Li, Zijian, and Dai, Y. Sophia

Published
2021
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31. S℡LAR MASS-GAS-PHASE METALLICITY RELATION AT 0.5 \textless= z \textless= 0.7: A POWER LAW WITH INCREASING SCATTER TOWARD THE LOW-MASS REGIME

Author

Trump, Jonathan R., Amorin, Ricardo, Barro, Guillermo, Dave, Romeel, Faber, S. M., Hathi, Nimish P., Yesuf, Hassen, Cooper, Michael C., Dekel, Avishai, Guhathakurta, Puragra, Kirby, Evan N., Koekemoer, Anton M., Perez-Gonzalez, Pablo G., Lin, Lihwai, Newman, Jeffery A., Primack, Joel R., Rosario, David J., Willmer, Christopher N. A., Yan, Renbin, Guo, Yicheng, Koo, David C., Lu, Yu, Forbes, John C., Rafelski, Marc, UCO/Lick Observatory, University of California [Santa Cruz] (UCSC), University of California-University of California, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Dalhousie University [Halifax], Racah Institute of Physics, The Hebrew University of Jerusalem (HUJ), Department of Chemical and Biomolecular Engineering, State Key Laboratory in Computer Science [Beijing] (SKLCS), Institute of Software Chinese Academy of Sciences [Beijing], AUTRES, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), and University of California (UC)-University of California (UC)

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

International audience; We present the stellar mass (M-*)-gas-phase metallicity relation (MZR) and its scatter at intermediate redshifts (0.5 \textless= z \textless= 0.7) for 1381 field galaxies collected from deep spectroscopic surveys. The star formation rate (SFR) and color at a given M-* of this magnitude-limited (R less than or similar to 24 AB) sample are representative of normal star-forming galaxies. For masses below 10(9) M-circle dot, our sample of 237 galaxies is similar to 10 times larger than those in previous studies beyond the local universe. This huge gain in sample size enables superior constraints on the MZR and its scatter in the low-mass regime. We find a power-law MZR at 10(8) M-circle dot \textless M-* \textless 10(11) M-circle dot: 12 + log (O/H) = (5.83 +/- 0.19)+(0.30 +/- 0.02) log (M-*/M-circle dot). At 10(9) M-circle dot \textless M-* \textless 10(10.5) M-circle dot, our MZR shows agreement with others measured at similar redshifts in the literature. Our power-law slope is, however, shallower than the extrapolation of the MZRs of others to masses below 10(9) M-circle dot. The SFR dependence of the MZR in our sample is weaker than that found for local galaxies (known as the fundamental metallicity relation). Compared to a variety of theoretical models, the slope of our MZR for low-mass galaxies agrees well with predictions incorporating supernova energy-driven winds. Being robust against currently uncertain metallicity calibrations, the scatter of the MZR serves as a powerful diagnostic of the stochastic history of gas accretion, gas recycling, and star formation of low-mass galaxies. Our major result is that the scatter of our MZR increases as M-* decreases. Our result implies that either the scatter of the baryonic accretion rate (sigma((M) over dot)) or the scatter of the M-*-M-halo relation (sigma(SHMR)) increases as M-* decreases. Moreover, our measure of scatter at z = 0.7 appears consistent with that found for local galaxies. This lack of redshift evolution constrains models of galaxy evolution to have both sigma((M) over dot) and sigma(SHMR) remain unchanged from z = 0.7 to z = 0.

Published
2016

32. Guitarra, a Simulator for the JWST/NIRCam.

Author

Willmer, Christopher N. A., Hainline, Kevin N., Curtis-Lake, Emma, da Cunha, Elisabete, Hodge, Jacqueline, Afonso, José, Pentericci, Laura, and Sobral, David

Abstract

We present an overview of Guitarra, a simulator for the Near Infrared Camera that creates scenes from catalogues of mock or real sources using the current best estimates of the instrument characteristics and the pattern on the sky of the observations. [ABSTRACT FROM AUTHOR]

Published
2020
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33. Warm-hot gas in X-ray bright galaxy clusters and the H I-deficient circumgalactic medium in dense environments.

Author

Burchett, Joseph N., Tripp, Todd M., Wang, Q. Daniel, Willmer, Christopher N. A., Bowen, David V., and Jenkins, Edward B.

Subjects
GALAXY clusters, CIRCUMSTELLAR matter, X-ray detection, QUASARS, SIGNAL-to-noise ratio
Abstract

We analyse the intracluster medium (ICM) and circumgalactic medium (CGM) in seven X-ray-detected galaxy clusters using spectra of background quasi-stellar objects (QSOs) (HSTCOS/ STIS), optical spectroscopy of the cluster galaxies (MMT/Hectospec and SDSS), and X-ray imaging/spectroscopy (XMM-Newton and Chandra). First, we report a very low covering fraction of HI absorption in the CGM of these cluster galaxies, fc = 25+25 per cent, to stringent detection limits (N(H I) <10-15 per cent, to stringent detection limits (N(H I) <1013 cm-2). As field galaxies have an HI covering fraction of ~100 per cent at similar radii, the dearth of CGM HI in our data indicates that the cluster environment has effectively stripped or overionized the gaseous haloes of these cluster galaxies. Secondly, we assess the contribution of warm-hot (105-106 K) gas to the ICM as traced by OVI and broad Ly α (BLA) absorption. Despite the high signal-to-noise ratio of our data, we do not detect OVI in any cluster, and we only detect BLA features in the QSO spectrum probing one cluster. We estimate that the total column density of warm-hot gas along this line of sight totals to ~3 per cent of that contained in the hot T > 107 K X-ray emitting phase. Residing at high relative velocities, these features may trace pre-shocked material outside the cluster. Comparing gaseous galaxy haloes from the low-density 'field' to galaxy groups and high-density clusters, we find that the CGM is progressively depleted of HI with increasing environmental density, and the CGM is most severely transformed in galaxy clusters. This CGM transformation may play a key role in environmental galaxy quenching. [ABSTRACT FROM AUTHOR]

Published
2018
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34. AKARI Observation of the North Ecliptic Pole (NEP) Supercluster at z = 0.087: Mid-infrared View of Transition Galaxies

Author

Ko, Jongwan, Im, Myungshin, Lee, Hyung Mok, Lee, Myung Gyoon, Kim, Seong Jin, Shim, Hyunjin, Jeon, Yiseul, Hwang, Ho Seong, Willmer, Christopher N. A., Malkan, Matthew A., Papovich, Casey, Weiner, Benjamin J., Matsuhara, Hideo, Oyabu, Shinki, and Takagi, Toshinobu

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, Mid infrared, FOS: Physical sciences, Ecliptic pole, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Physical Chemistry, galaxies [infrared], Atomic, Morphological transformation, Particle and Plasma Physics, surveys, Supercluster, clusters: general [galaxies], Astrophysics::Solar and Stellar Astrophysics, Nuclear, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, Star formation, Molecular, Astronomy and Astrophysics, stellar content [galaxies], Galaxy, Space and Planetary Science, astro-ph.CO, Astrophysics::Earth and Planetary Astrophysics, Astronomical and Space Sciences, Dust emission, Physical Chemistry (incl. Structural), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数: 15名, Accepted: 2011-11-28, 資料番号: SA1003019000

Published
2012

36. The DEEP3 Galaxy Redshift Survey: The Impact of Environment on the Size Evolution of Massive Early-type Galaxies at Intermediate Redshift

Author

Cooper, Michael C., Griffith, Roger L., Newman, Jeffrey A., Coil, Alison L., Davis, Marc, Dutton, Aaron A., Faber, S. M., Guhathakurta, Puragra, Koo, David C., Lotz, Jennifer M., Weiner, Benjamin J., Willmer, Christopher N. A., and Yan, Renbin

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using data drawn from the DEEP2 and DEEP3 Galaxy Redshift Surveys, we investigate the relationship between the environment and the structure of galaxies residing on the red sequence at intermediate redshift. Within the massive (10 < log(M*/Msun) < 11) early-type population at 0.4 < z, 11 pages, 5 figures, 2 tables; resubmitted to MNRAS after addressing referee's comments (originally submitted to journal on August 16, 2011)

Published
2011

37. How does galaxy environment matter? The relationship between galaxy environments, colour and stellar mass at 0.4 < z < 1 in the Palomar/DEEP2 survey

Author

Grützbauch, Ruth, Conselice, Christopher J., Varela, Jesús, Bundy, Kevin, Cooper, Michael C., Skibba, Ramin, and Willmer, Christopher N. A.

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a study characterizing the environments of galaxies in the redshift range of 0.4 < z < 1 based on data from the POWIR near infrared imaging and DEEP2 spectroscopic redshift surveys, down to a stellar mass of log M* = 10.25 M_sun. Galaxy environments are measured in terms of nearest neighbour densities as well as fixed aperture densities and kinematical and dynamical parameters of neighbour galaxies within a radius of 1 Mpc. We disentangle the correlations between galaxy stellar mass, galaxy colour and galaxy environment, using not only galaxy number densities, but also other environmental characteristics such as velocity dispersion, mean harmonic radius, and crossing time. We find that galaxy colour and the fraction of blue galaxies depends very strongly on stellar mass at 0.4 < z < 1, while a weak additional dependence on local number densities is in place at lower redshifts (0.4 < z < 0.7). This environmental influence is most visible in the colours of intermediate mass galaxies (10.5 < log M* < 11), whereas colours of lower and higher mass galaxies remain largely unchanged with redshift and environment. At a fixed stellar mass, the colour-density relation almost disappears, while the colour-stellar mass relation is present at all local densities. We find a weak correlation between stellar mass and environment at intermediate redshifts, which contributes to the overall colour-density relation. We furthermore do not find a significant correlation between galaxy colour and virial mass, i.e., parent dark matter halo mass. Galaxy stellar mass thus appears to be the crucial defining parameter for intrinsic galaxy properties such as ongoing star formation and colour., Comment: 20 pages, 13 figures, accepted for publication in MNRAS

Published
2010

38. A Strong-Lens Survey in AEGIS: the influence of large scale structure

Author

Moustakas, Leonidas A., Marshall, Phil, Newman, Jeffrey A., Coil, Alison L., Cooper, Michael C., Davis, Marc, Fassnacht, Christopher D., Guhathakurta, Puragra, Hopkins, Andrew, Koekemoer, Anton, Konidaris, Nicholas P., Lotz, Jennifer M., and Willmer, Christopher N. A.

Subjects
Physics, Galaxies gravitational lensing
Published
2008

39. The DEEP Groth Strip Survey VI. Spectroscopic, Variability, and X-ray Detection of AGN

Author

Sarajedini, Vicki L., Koo, David C., Phillips, Andrew C., Kobulnicky, Henry A., Gebhardt, Karl, Willmer, Christopher N. A., Vogt, Nicole P., Laird, Elise, Im, Myungshin, Iverson, Sarah, and Mattos, Wanessa

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We identify active galactic nuclei (AGN) in the Groth-Westphal Survey Strip (GSS) using the independent and complementary selection techniques of optical spectroscopy and photometric variability. We discuss the X-ray properties of these AGN using Chandra/XMM data for this region. From a sample of 576 galaxies with high quality spectra we identify 31 galaxies with AGN signatures. Seven of these have broad emission lines (Type 1 AGNs). We also identify 26 galaxies displaying nuclear variability in HST WFPC2 images of the GSS separated by ~7 years. The primary overlap of the two selected AGN samples is the set of broad-line AGNs, of which 80% appear as variable. Only a few narrow-line AGNs approach the variability threshold. The broad-line AGNs have an average redshift of z~1.1 while the other spectroscopic AGNs have redshifts closer to the mean of the general galaxy population (z~0.7). Eighty percent of the identified broad-line AGNs are detected in X-rays and these are among the most luminous X-ray sources in the GSS. Only one narrow-line AGN is X-ray detected. Of the variable nuclei galaxies within the X-ray survey, 27% are X-ray detected. We find that 1.9+/-0.6% of GSS galaxies to V=24 are broad-line AGNs, 1.4+/-0.5% are narrow-line AGNs, and 4.5+/-1.4% contain variable nuclei. The fraction of spectroscopically identified BLAGNs and NLAGNs at z~1 reveals a marginally significant increase of 1.3+/-0.9% when compared to the local population., 29 pages, 8 figures, accepted for publication in ApJS

Published
2006

40. The DEEP Groth Strip Galaxy Redshift Survey. VIII. The Evolution of Luminous Field Bulges at Redshift z ~ 1

Author

Koo, David C., Simard, Luc, Willmer, Christopher N. A., Gebhardt, Karl, Bouwens, Rychard J., Kauffmann, Guinevere, Crosby, Timothy, Faber, S. M., Sarajedini, Vicki L., Vogt, Nicole P., Weiner, Benjamin J., Phillips, A. C., Im, Myungshin, and Wu, K. L.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present a sample of over 50 luminous field bulges (including ellipticals) found in the Groth Strip Survey (GSS), with 0.73< z < 1.04 and with bulge magnitudes I, ApJS accepted, 106 pages, 10 figures. Figure 14 in JPEG format. Full version available at http://deep.ucolick.org/publications.html

Published
2004

41. Are There Blue, Massive E/S0s at z < 1 ?: Kinematics of Blue Spheroidal Galaxy Candidates

Author

Im, Myungshin, Faber, S. M., Gebhardt, Karl, Koo, David C., Phillips, Andrew C., Schiavon, Ricardo P., Simard, Luc, and Willmer, Christopher N. A.

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Several recent studies find that 10 - 50% of morphologically selected field early-type galaxies at redshifts z, Comment: Accepted for publication in the Astronomical Journal

Published
2001

42. Direct determination of oxygen abundances in line-emitting star-forming galaxies at intermediate redshift.

Author

Pérez, José M., Hoyos, Carlos, Díaz, Ángeles I., Koo, David C., and Willmer, Christopher N. A.

Subjects
GALAXIES, ASTRONOMY, REDSHIFT, TIDAL stripping (Astrophysics), CHALCOGENS
Abstract

We present a sample of 22 blue [(B - V)AB < 0.45], luminous (MB,AB < -18.9), metal-poor galaxies in the 0.69☉ and 1/3 Z☉. We find that galaxies in our sample have comparablemetallicities to other intermediate-redshift samples, but are more metal poor than local systems of similar B-band luminosities and star formation activity. The galaxies here show similar properties to the green peas discovered at z ≃ 0.2-0.3, though our galaxies tend to be slightly less luminous. [ABSTRACT FROM AUTHOR]

Published
2016
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43. Dependence of galaxy quenching on halo mass and distance from its centre.

Author

Woo, Joanna, Dekel, Avishai, Faber, S. M., Noeske, Kai, Koo, David C., Gerke, Brian F., Cooper, Michael C., Salim, Samir, Dutton, Aaron A., Newman, Jeffrey, Weiner, Benjamin J., Bundy, Kevin, Willmer, Christopher N. A., Davis, Marc, and Yan, Renbin

Subjects
STAR formation, GALACTIC halos, ATOMIC mass, STAR colors, GALACTIC evolution
Abstract

We study the dependence of star formation quenching on galaxy mass and environment, in the Sloan Digital Sky Survey (SDSS; z ∼ 0.1) and the All-Wavelength Extended Groth Strip International Survey (AEGIS; z ∼ 1). It is crucial that we define quenching by low star formation rate rather than by red colour, given that one-third of the red galaxies are star forming. We address stellar mass M*, halo mass Mh, density over the nearest N neighbours δN and distance to the halo centre D. The fraction of quenched galaxies appears more strongly correlated with Mh at fixed M* than with M* at fixed Mh, while for satellites quenching also depends on D. We present the M*–Mh relation for centrals at z ∼ 1. At z ∼ 1, the dependence of quenching on M* at fixed Mh is somewhat more pronounced than at z ∼ 0, but the quenched fraction is low (10 per cent) and the haloes are less massive. For satellites, M*-dependent quenching is noticeable at high D, suggesting a quenching dependence on subhalo mass for recently captured satellites. At small D, where satellites likely fell in more than a few Gyr ago, quenching strongly depends on Mh and not on M*. The Mh dependence of quenching is consistent with theoretical wisdom where virial shock heating in massive haloes shuts down accretion and triggers ram-pressure stripping, causing quenching. The interpretation of δN is complicated by the fact that it depends on the number of observed group members compared to N, motivating the use of D as a better measure of local environment. [ABSTRACT FROM AUTHOR]

Published
2013
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44. The Arizona CDFS Environment Survey (ACES): A Magellan/IMACS Spectroscopic Survey of the Chandra Deep Field-South The Arizona CDFS Environment Survey (ACES): A Magellan/IMACS Spectroscopic Survey of the Chandra Deep Field-South.

Author

Cooper, Michael C., Yan, Renbin, Dickinson, Mark, Juneau, Stéphanie, Lotz, Jennifer M., Newman, Jeffrey A., Papovich, Casey, Salim, Samir, Walth, Gregory, Weiner, Benjamin J., and Willmer, Christopher N. A.

Subjects
GALACTIC redshift, SURVEYS, ASTRONOMICAL photometry, ASTRONOMICAL observations, SAMPLING theorem, IMAGING systems in astronomy
Abstract

ABSTRACT We present the Arizona CDFS Environment Survey (ACES), a recently completed spectroscopic redshift survey of the Chandra Deep Field-South (CDFS) conducted using the Inamori-Magellan Areal Camera and Spectrograph on the Magellan-Baade telescope. In total, the survey targeted 7277 unique sources down to a limiting magnitude of RAB = 24.1, yielding 5080 secure redshifts across the ∼30 arcmin × 30 arcmin extended CDFS region. The ACES data set delivers a significant increase to both the spatial coverage and the sampling density of the spectroscopic observations in the field. Combined with previously published spectroscopic redshifts, ACES now creates a highly complete survey of the galaxy population at R < 23, enabling the local galaxy density (or environment) on relatively small scales (∼1 Mpc) to be measured at z < 1 in one of the most heavily studied and data-rich fields in the sky. Here, we describe the motivation, design and implementation of the survey and present a preliminary redshift and environment catalogue. In addition, we utilize the ACES spectroscopic redshift catalogue to assess the quality of photometric redshifts from both the COMBO-17 and Multiwavelength Survey by Yale-Chile imaging surveys of the CDFS. [ABSTRACT FROM AUTHOR]

Published
2012
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45. The DEEP3 Galaxy Redshift Survey: the impact of environment on the size evolution of massive early-type galaxies at intermediate redshift.

Author

Cooper, Michael C., Griffith, Roger L., Newman, Jeffrey A., Coil, Alison L., Davis, Marc, Dutton, Aaron A., Faber, S. M., Guhathakurta, Puragra, Koo, David C., Lotz, Jennifer M., Weiner, Benjamin J., Willmer, Christopher N. A., and Yan, Renbin

Subjects
REDSHIFT, GALACTIC evolution, SURVEYS, DATA analysis, STATISTICAL correlation, STELLAR mass, ASTRONOMICAL observations, QUASARS
Abstract

ABSTRACT Using data drawn from the DEEP2 and DEEP3 Galaxy Redshift Surveys, we investigate the relationship between the environment and the structure of galaxies residing on the red sequence at intermediate redshift. Within the massive (10 < log10( M★/ h−2 M⊙) < 11) early-type population at 0.4 < z < 1.2, we find a significant correlation between local galaxy overdensity (or environment) and galaxy size, such that early-type systems in higher density regions tend to have larger effective radii (by ∼0.5 h−1 kpc or 25 per cent larger) than their counterparts of equal stellar mass and Sérsic index in lower density environments. This observed size-density relation is consistent with a model of galaxy formation in which the evolution of early-type systems at z < 2 is accelerated in high-density environments such as groups and clusters and in which dry, minor mergers (versus mechanisms such as quasar feedback) play a central role in the structural evolution of the massive, early-type galaxy population. [ABSTRACT FROM AUTHOR]

Published
2012
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46. AKARI OBSERVATION OF THE NORTH ECLIPTIC POLE (NEP) SUPERCLUSTER AT z = 0.087: MID-INFRARED VIEW OF TRANSITION GALAXIES.

Author

Jongwan ko, Myungshin Im, Hyung Mok Lee, Myung Gyoon Lee, Seong Jin Kim, Hyunjin Shim, Yiseul Jeon, Ho Seong Hwang, Willmer, Christopher N. A., Malkan, Matthew A., Papovich, Casey, Weiner, Benjamin J., Matsuhara, Hideo, Oyabu, Shinki, and Takagi, Toshinobu

Subjects
GALAXY clusters, GALACTIC evolution, STAR formation, STELLAR populations, STELLAR mass
Abstract

We present the mid-infrared (MIR) properties of galaxies within a supercluster in the north ecliptic pole region at z ~ 0.087 observed with the AKARI satellite. We use data from the AKARI NEP-Wide (5.4 deg²) IR survey and the CLusters of galaxies EVoLution studies (CLEVL) mission program. We show that near-IR (3 µm)-mid-IR (11 µm) color can be used as an indicator of the specific star formation rate and the presence of intermediate-age stellar populations. From the MIR observations, we find that red-sequence galaxies consist not only of passively evolving red early-type galaxies, but also of (1) "weak-SFGs" (disk-dominated star-forming galaxies that have star formation rates lower by ~4 x than blue-cloud galaxies) and (2) "intermediate-MXGs" (bulge-dominated galaxies showing stronger MIR dust emission than normal red early-type galaxies). These two populations can be a set of transition galaxies from blue, star-forming, late-type galaxies evolving into red, quiescent, early-type ones. We find that the weak-SFGs are predominant at intermediate masses (1010 M⊙ < M* < 1010.5 M⊙) and are typically found in local densities similar to the outskirts of galaxy clusters. As much as 40% of the supercluster member galaxies in this mass range can be classified as weak-SFGs, but their proportion decreases to <10% at larger masses (M* > 1010.5 M⊙) at any galaxy density. The fraction of the intermediate-MXG among red-sequence galaxies at 1010 M⊙ < M* < 1011 M⊙ also decreases as the density and mass increase. In particular, ~42% of the red-sequence galaxies with early-type morphologies are classified as intermediate-MXGs at intermediate densities. These results suggest that the star formation activity is strongly dependent on the stellar mass, but that the morphological transformation is mainly controlled by the environment. [ABSTRACT FROM AUTHOR]

Published
2012
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47. Autocorrelations of stellar light and mass at z∼ 0 and ∼1: from SDSS to DEEP2.

Author

Li, Cheng, White, Simon D. M., Chen, Yanmei, Coil, Alison L., Davis, Marc, De Lucia, Gabriella, Guo, Qi, Jing, Y. P., Kauffmann, Guinevere, Willmer, Christopher N. A., and Zhang, Wei

Subjects
AUTOCORRELATION (Statistics), STELLAR luminosity function, STELLAR mass, DARK matter, REDSHIFT, GALAXY clusters
Abstract

ABSTRACT We present measurements of projected autocorrelation functions wp( rp) for the stellar mass of galaxies and for their light in the U, B and V bands, using data from the third data release of the DEEP2 Galaxy Redshift Survey and the final data release of the Sloan Digital Sky Survey (SDSS). We investigate the clustering bias of stellar mass and light by comparing these to projected autocorrelations of dark matter estimated from the Millennium Simulations (MS) at z= 1 and 0.07, the median redshifts of our galaxy samples. All of the autocorrelation and bias functions show systematic trends with spatial scale and waveband which are impressively similar at the two redshifts. This shows that the well-established environmental dependence of stellar populations in the local Universe is already in place at z= 1. The recent MS-based galaxy formation simulation of reproduces the scale-dependent clustering of luminosity to an accuracy better than 30 per cent in all bands and at both redshifts, but substantially overpredicts mass autocorrelations at separations below about 2 Mpc. Further comparison of the shapes of our stellar mass bias functions with those predicted by the model suggests that both the SDSS and DEEP2 data prefer a fluctuation amplitude of σ8∼ 0.8 rather than the σ8= 0.9 assumed by the MS. [ABSTRACT FROM AUTHOR]

Published
2012
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48. PROBING THE STAR FORMATION HISTORY AND INITIAL MASS FUNCTION OF THE Z &#x223c: 2.5 LENSED GALAXY SMM J163554.2+661225 WITH HERSCHEL.

Author

Finkelstein, Keely D., Papovich, Casey, Finkelstein, Steven L., Willmer, Christopher N. A., Rigby, Jane R., Rudnick, Gregory, Egami, Eiichi, Rieke, Marcia, and Smith, J.-D. T.

Subjects
STAR formation, STELLAR initial mass function, ASTRONOMICAL photometry, SPECTRAL energy distribution, REDSHIFT
Abstract

We present the analysis of Herschel Spectral and Photometric Imaging Receiver far-infrared (FIR) observations of the z = 2.515 tensed galaxy SMM J163554.2+661225. Combining new 250, 350, and 500 µm observations with existing data, we make an improved fit to the FIR spectral energy distribution of this galaxy. We find a total infrared (IR) luminosity of L(8-1000 µm) =6.9 ± 0.6 x 1011 L⊙, a factor of three more precise over previous LIR estimates for this galaxy, and one of the most accurate measurements for any galaxy at these redshifts. This FIR luminosity implies an unlensed star formation rate (SFR) for this galaxy of 119 ± 10 M⊙ yr-1, which is a factor of 1.9 ± 0.35 lower than the SFR derived from the nebular Paα emission line (a 2.5σ discrepancy). Both SFR indicators assume an identical Salpeter initial mass function (IMF) with slope Γ = 2.35 over a mass range of 0.1-100 M⊙; thus this discrepancy suggests that more ionizing photons may be necessary to account for the higher Paα-derived SFR. We examine a number of scenarios and find that the observations can be explained with a varying star formation history (SFH) due to an increasing SFR, paired with a slight flattening of the IMF. If the SFR is constant in time, then larger changes need to be made to the IMF by either increasing the upper mass cutoff to ~200 M⊙, or a flattening of the IMF slope to 1.9 ± 0.15, or a combination of the two. These scenarios result in up to double the number of Stars with masses above 20 M⊙, which produce the requisite increase in ionizing photons over a Salpeter IMF with a constant SFH. [ABSTRACT FROM AUTHOR]

Published
2011
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49. How does galaxy environment matter? The relationship between galaxy environments, colour and stellar mass at 0.4 < z < 1 in the Palomar/DEEP2 survey.

Author

Grützbauch, Ruth, Conselice, Christopher J., Varela, Jesús, Bundy, Kevin, Cooper, Michael C., Skibba, Ramin, and Willmer, Christopher N. A.

Subjects
GALACTIC dynamics, STELLAR mass, STAR colors, STAR formation, REDSHIFT, NEAR infrared spectroscopy, INFRARED imaging
Abstract

We present a study characterizing the environments of galaxies in the redshift range of based on data from the POWIR near-infrared imaging and DEEP2 spectroscopic redshift surveys, down to a stellar mass of . Galaxy environments are measured in terms of nearest-neighbour densities as well as fixed aperture densities and kinematical and dynamical parameters of neighbour galaxies within a radius of Mpc. We disentangle the correlations between galaxy stellar mass, galaxy colour and galaxy environment, using not only galaxy number densities, but also other environmental characteristics such as velocity dispersion, mean harmonic radius and crossing time. We find that galaxy colour and the fraction of blue galaxies depends very strongly on stellar mass at , while a weak additional dependence on local number densities is in place at lower redshifts . This environmental influence is most visible in the colours of intermediate-mass galaxies , whereas colours of lower- and higher-mass galaxies remain largely unchanged with redshift and environment. At a fixed stellar mass, the colour-density relation almost disappears, while the colour-stellar mass relation is present at all local densities. We find a weak correlation between stellar mass and environment at intermediate redshifts, which contributes to the overall colour-density relation. We furthermore do not find a significant correlation between galaxy colour and virial mass, i.e. parent dark matter halo mass. Galaxy stellar mass thus appears to be the crucial defining parameter for intrinsic galaxy properties such as ongoing star formation and colour. [ABSTRACT FROM AUTHOR]

Published
2011
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50. Absence of evidence is not evidence of absence: the colour-density relation at fixed stellar mass persists to z∼ 1 Absence of evidence is not evidence of absence: the colour-density relation at fixed stellar mass persists to z∼ 1 M. C. Cooper et al. Absence of evidence/evidence of absence

Author

Cooper, Michael C., Coil, Alison L., Gerke, Brian F., Newman, Jeffrey A., Bundy, Kevin, Conselice, Christopher J., Croton, Darren J., Davis, Marc, Faber, S. M., Guhathakurta, Puragra, Koo, David C., Lihwai Lin, Weiner, Benjamin J., Willmer, Christopher N. A., and Yan, Renbin

Subjects
GALAXIES, STELLAR mass, ASTRONOMY, UNIVERSE, STATISTICS
Abstract

We use data drawn from the DEEP2 Galaxy Redshift Survey to investigate the relationship between local galaxy density, stellar mass and rest-frame galaxy colour. At , we find that the shape of the stellar mass function at the high-mass end depends on the local environment, with high-density regions favouring more massive systems. Accounting for this stellar mass-environment relation (i.e. working at fixed stellar mass), we find a significant colour-density relation for galaxies with and . This result is shown to be robust to variations in the sample selection and to extend to even lower masses [down to ]. We conclude by discussing our results in comparison to recent works in the literature, which report no significant correlation between galaxy properties and environment at fixed stellar mass for the same redshift and stellar mass domain. The non-detection of environmental dependence found in other data sets is largely attributable to their smaller sample sizes and lower sampling density, as well as systematic effects such as inaccurate redshifts and biased analysis techniques. Ultimately, our results based on DEEP2 data illustrate that the evolutionary state of a galaxy at is not exclusively determined by the stellar mass of the galaxy. Instead, we show that local environment appears to play a distinct role in the transformation of galaxy properties at . [ABSTRACT FROM AUTHOR]

Published
2010
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