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  • 1
    Online Resource
    Online Resource
    X-Ray Emission from the Jets and Lobes of the Spiderweb
    American Astronomical Society ; 2022
    In:  The Astrophysical Journal Vol. 928, No. 1 ( 2022-03-01), p. 59-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 928, No. 1 ( 2022-03-01), p. 59-
    Abstract: Deep Chandra and Very Large Array imaging reveals a clear correlation between X-ray and radio emission on scales ∼100 kpc in the Spiderweb radio galaxy at z = 2.16. The X-ray emission associated with the extended radio source is likely dominated by inverse Compton upscattering of cosmic microwave background photons by the radio-emitting relativistic electrons. For regions dominated by high surface brightness emission, such as hot spots and jet knots, the implied magnetic fields are ∼50–70 μ G. The nonthermal pressure in these brighter regions is then ∼9 × 10 −10 dynes cm −2 , or three times larger than the nonthermal pressure derived assuming minimum energy conditions, and an order of magnitude larger than the thermal pressure in the ambient cluster medium. Assuming ram pressure confinement implies an average advance speed for the radio source of ∼2400 km s −1 and a source age of ∼3 × 10 7 yr. Considering the lower surface brightness, diffuse radio-emitting regions, we identify an evacuated cavity in the Ly α emission coincident with the tail of the eastern radio lobe. Making reasonable assumptions for the radio spectrum, we find that the relativistic electrons and fields in the lobe are plausibly in pressure equilibrium with the thermal gas and close to a minimum energy configuration. The radio morphology suggests that the Spiderweb is a high- z example of the rare class of hybrid morphology radio sources (or HyMoRS), which we attribute to interaction with the asymmetric gaseous environment indicated by the Ly α emission.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/ac55a0
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2022
    detail.hit.zdb_id: 2960-9
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 2
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    Hidden in Plain Sight: A Massive, Dusty Starburst in a Galaxy Protocluster at z = 5.7 in the COSMOS Field
    American Astronomical Society ; 2018
    In:  The Astrophysical Journal Vol. 861, No. 1 ( 2018-07-01), p. 43-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 861, No. 1 ( 2018-07-01), p. 43-
    Abstract: We report the serendipitous discovery of a dusty, starbursting galaxy at z  = 5.667 (hereafter called CRLE) in close physical association with the “normal” main-sequence galaxy HZ10 at z  = 5.654. CRLE was identified by detection of [C ii ], [N ii ], and CO(2–1) line emission, making it the highest-redshift, most luminous starburst in the COSMOS field. This massive, dusty galaxy appears to be forming stars at a rate of at least 1500 M ⊙ yr −1 in a compact region only ∼3 kpc in diameter. The dynamical and dust emission properties of CRLE suggest an ongoing merger driving the starburst, which is in a potentially intermediate stage relative to other known dusty galaxies at the same epoch. The ratio of [C ii ] to [N ii ] may suggest that an important (∼15%) contribution to the [C ii ] emission comes from a diffuse ionized gas component, which could be more extended than the dense, starbursting gas. CRLE appears to be located in a significant galaxy overdensity at the same redshift, potentially associated with a large-scale cosmic structure recently identified in a Lyman α -emitter survey. This overdensity suggests that CRLE and HZ10 reside in a protocluster environment, offering the tantalizing opportunity to study the effect of a massive starburst on protocluster star formation. Our findings support the interpretation that a significant fraction of the earliest galaxy formation may occur from the inside out, within the central regions of the most massive halos, while rapidly evolving into the massive galaxy clusters observed in the local universe.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/aac6b6
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2018
    detail.hit.zdb_id: 2960-9
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 3
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    COLDz: A High Space Density of Massive Dusty Starburst Galaxies ∼1 Billion Years after the Big Bang
    American Astronomical Society ; 2020
    In:  The Astrophysical Journal Vol. 895, No. 2 ( 2020-06-01), p. 81-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 895, No. 2 ( 2020-06-01), p. 81-
    Abstract: We report the detection of CO( J  = 2 → 1) emission from three massive dusty starburst galaxies at z   〉  5 through molecular line scans in the NSF’s Karl G. Jansky Very Large Array (VLA) CO Luminosity Density at High Redshift (COLDz) survey. Redshifts for two of the sources, HDF 850.1 ( z  = 5.183) and AzTEC-3 ( z  = 5.298), were previously known. We revise a previous redshift estimate for the third source GN10 ( z  = 5.303), which we have independently confirmed through detections of CO J  = 1 → 0, 5 → 4, 6 → 5, and [C ii ] 158 μ m emission with the VLA and the NOrthern Extended Milllimeter Array. We find that two currently independently confirmed CO sources in COLDz are “optically dark”, and that three of them are dust-obscured galaxies at z   〉  5. Given our survey area of ∼60 arcmin 2 , our results appear to imply a ∼6–55 times higher space density of such distant dusty systems within the first billion years after the Big Bang than previously thought. At least two of these z   〉  5 galaxies show star formation rate surface densities consistent with so-called “maximum” starbursts, but we find significant differences in CO excitation between them. This result may suggest that different fractions of the massive gas reservoirs are located in the dense, star-forming nuclear regions—consistent with the more extended sizes of the [C ii ] emission compared to the dust continuum and higher [C ii ]-to-far-infrared luminosity ratios in those galaxies with lower gas excitation. We thus find substantial variations in the conditions for star formation between z   〉  5 dusty starbursts, which typically have dust temperatures that are ∼57% ± 25% warmer than starbursts at z  = 2–3 due to their enhanced star formation activity.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/ab8c48
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2020
    detail.hit.zdb_id: 2960-9
    detail.hit.zdb_id: 1473835-1
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  • 4
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    Online Resource
    HIGH-SENSITIVITY ARRAY OBSERVATIONS OF THE z = 1.87 SUBMILLIMETER GALAXY GOODS 850-3
    American Astronomical Society ; 2010
    In:  The Astronomical Journal Vol. 139, No. 4 ( 2010-04-01), p. 1622-1627
    Details
    In: The Astronomical Journal, American Astronomical Society, Vol. 139, No. 4 ( 2010-04-01), p. 1622-1627
    Type of Medium: Online Resource
    ISSN: 0004-6256 , 1538-3881
    URL: Article
    DOI: 10.1088/0004-6256/139/4/1622
    RVK:
    US 1090
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2010
    detail.hit.zdb_id: 127191-X
    detail.hit.zdb_id: 2003104-X
    SSG: 16,12
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  • 5
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    ALMA IMAGING OF GAS AND DUST IN A GALAXY PROTOCLUSTER AT REDSHIFT 5.3: [C II] EMISSION IN “TYPICAL” GALAXIES AND DUSTY STARBURSTS ≈1 BILLION YEARS AFTER THE BIG BANG
    American Astronomical Society ; 2014
    In:  The Astrophysical Journal Vol. 796, No. 2 ( 2014-11-10), p. 84-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 796, No. 2 ( 2014-11-10), p. 84-
    Type of Medium: Online Resource
    ISSN: 1538-4357
    URL: Article
    DOI: 10.1088/0004-637X/796/2/84
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2014
    detail.hit.zdb_id: 1473835-1
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  • 6
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    ALMA REVEALS WEAK [N ii] EMISSION IN “TYPICAL” GALAXIES AND INTENSE STARBURSTS AT z = 5–6
    American Astronomical Society ; 2016
    In:  The Astrophysical Journal Vol. 832, No. 2 ( 2016-12-01), p. 151-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 832, No. 2 ( 2016-12-01), p. 151-
    Abstract: We report interferometric measurements of [N ii ] 205 μ m fine-structure line emission from a representative sample of three galaxies at z  = 5–6 using the Atacama Large (sub)Millimeter Array (ALMA). These galaxies were previously detected in [C ii ] and far-infrared continuum emission and span almost two orders of magnitude in star formation rate (SFR). Our results show at least two different regimes of ionized interstellar medium properties for galaxies in the first billion years of cosmic time, separated by their ratio. We find extremely low [N ii ] e mission compared to [C ii ] ( ) from a “typical” star-forming galaxy, likely directly or indirectly (by its effect on the radiation field) related to low dust abundance and low metallicity. The infrared-luminous modestly star-forming Lyman-break galaxy (LBG) in our sample is characterized by an ionized-gas fraction ( typical of local star-forming galaxies and shows evidence for spatial variations in its ionized-gas fraction across an extended gas reservoir. The extreme SFR, warm and compact dusty starburst AzTEC-3 shows an ionized fraction higher than expected given its SFR surface density ( ) suggesting that [N ii ] dominantly traces a diffuse ionized medium rather than star-forming H ii regions in this type of galaxy. This highest redshift sample of [N ii ] detections provides some of the first constraints on ionized and neutral gas modeling attempts and on the structure of the interstellar medium at z  = 5–6 in “normal” galaxies and starbursts.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/0004-637X/832/2/151
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2016
    detail.hit.zdb_id: 2960-9
    detail.hit.zdb_id: 1473835-1
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  • 7
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    Online Resource
    COLDz: Shape of the CO Luminosity Function at High Redshift and the Cold Gas History of the Universe
    American Astronomical Society ; 2019
    In:  The Astrophysical Journal Vol. 872, No. 1 ( 2019-02-10), p. 7-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 872, No. 1 ( 2019-02-10), p. 7-
    Abstract: We report the first detailed measurement of the shape of the CO luminosity function at high redshift, based on 〉 320 hr of the NSF’s Karl G. Jansky Very Large Array (VLA) observations over an area of ∼60 arcmin 2 taken as part of the CO Luminosity Density at High Redshift (COLDz) survey. COLDz “blindly” selects galaxies based on their cold gas content through CO( J  = 1 → 0) emission at z  ∼ 2–3 and CO( J  = 2 → 1) at z  ∼ 5–7 down to a CO luminosity limit of log( /K km s −1 pc 2 ) ≃ 9.5. We find that the characteristic luminosity and bright end of the CO luminosity function are substantially higher than predicted by semi-analytical models, but consistent with empirical estimates based on the infrared luminosity function at z  ∼ 2. We also present the currently most reliable measurement of the cosmic density of cold gas in galaxies at early epochs, i.e., the cold gas history of the universe, as determined over a large cosmic volume of ∼375,000 Mpc 3 . Our measurements are in agreement with an increase of the cold gas density from z  ∼ 0 to z  ∼ 2–3, followed by a possible decline toward z  ∼ 5–7. These findings are consistent with recent surveys based on higher- J CO line measurements, upon which COLDz improves in terms of statistical uncertainties by probing ∼50–100 times larger areas and in the reliability of total gas mass estimates by probing the low- J CO lines accessible to the VLA. Our results thus appear to suggest that the cosmic star formation rate density follows an increased cold molecular gas content in galaxies toward its peak about 10 billion years ago, and that its decline toward the earliest epochs is likely related to a lower overall amount of cold molecular gas (as traced by CO) bound in galaxies toward the first billion years after the Big Bang.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/aafc27
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2019
    detail.hit.zdb_id: 2960-9
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 8
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    Online Resource
    The Spiderweb Protocluster is Being Magnetized by Its Central Radio Jet
    American Astronomical Society ; 2022
    In:  The Astrophysical Journal Vol. 937, No. 1 ( 2022-09-01), p. 45-
    Details
    In: The Astrophysical Journal, American Astronomical Society, Vol. 937, No. 1 ( 2022-09-01), p. 45-
    Abstract: We present deep broadband radio polarization observations of the Spiderweb radio galaxy (J1140-2629) in a galaxy protocluster at z = 2.16. These yield the most detailed polarimetric maps yet made of a high-redshift radio galaxy. The intrinsic polarization angles and Faraday rotation measures (RMs) reveal coherent magnetic fields spanning the ∼60 kpc length of the jets, while ∼50% fractional polarizations indicate these fields are well ordered. Source-frame ∣RM∣ values of ∼1000 rad m −2 are typical, and values up to ∼11,100 rad m −2 are observed. The Faraday-rotating gas cannot be well mixed with the synchrotron-emitting gas, or stronger-than-observed depolarization would occur. Nevertheless, an observed spatial coincidence between a localized ∣RM∣ enhancement of ∼1100 rad m −2 , a bright knot of Ly α emission, and a deviation of the radio jet provide direct evidence for vigorous jet-gas interaction. We detect a large-scale RM gradient totaling ∼1000 s rad m −2 across the width of the jet, suggesting a net clockwise (as viewed from the active galactic nuclei) toroidal magnetic field component exists at tens-of-kiloparsec scales, which we speculate may be associated with the operation of a Poynting–Robertson cosmic battery. We conclude the RMs are mainly generated in a sheath of hot gas around the radio jet, rather than the ambient foreground protocluster gas. The estimated magnetic field strength decreases by successive orders of magnitude going from the jet hotspots (∼90 μ G) to the jet sheath (∼10 μ G) to the ambient intracluster medium (∼1 μ G). Synthesizing our results, we propose that the Spiderweb radio galaxy is actively magnetizing its surrounding protocluster environment, with possible implications for theories of the origin and evolution of cosmic magnetic fields.
    Type of Medium: Online Resource
    ISSN: 0004-637X , 1538-4357
    URL: Article
    DOI: 10.3847/1538-4357/ac7ec0
    RVK:
    UA 1000
    Language: Unknown
    Publisher: American Astronomical Society
    Publication Date: 2022
    detail.hit.zdb_id: 2960-9
    detail.hit.zdb_id: 1473835-1
    SSG: 16,12
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  • 9
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    Online Resource
    Foreground modelling via Gaussian process regression: an application to HERA data
    Oxford University Press (OUP) ; 2020
    In:  Monthly Notices of the Royal Astronomical Society Vol. 495, No. 3 ( 2020-07-01), p. 2813-2826
    Details
    In: Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP), Vol. 495, No. 3 ( 2020-07-01), p. 2813-2826
    Abstract: The key challenge in the observation of the redshifted 21-cm signal from cosmic reionization is its separation from the much brighter foreground emission. Such separation relies on the different spectral properties of the two components, although, in real life, the foreground intrinsic spectrum is often corrupted by the instrumental response, inducing systematic effects that can further jeopardize the measurement of the 21-cm signal. In this paper, we use Gaussian Process Regression to model both foreground emission and instrumental systematics in ∼2 h of data from the Hydrogen Epoch of Reionization Array. We find that a simple co-variance model with three components matches the data well, giving a residual power spectrum with white noise properties. These consist of an ‘intrinsic’ and instrumentally corrupted component with a coherence scale of 20 and 2.4 MHz, respectively (dominating the line-of-sight power spectrum over scales k∥ ≤ 0.2 h cMpc−1) and a baseline-dependent periodic signal with a period of ∼1 MHz (dominating over k∥ ∼ 0.4–0.8 h cMpc−1), which should be distinguishable from the 21-cm Epoch of Reionization signal whose typical coherence scale is ∼0.8 MHz.
    Type of Medium: Online Resource
    ISSN: 0035-8711 , 1365-2966
    URL: Article
    DOI: 10.1093/mnras/staa1331
    Language: English
    Publisher: Oxford University Press (OUP)
    Publication Date: 2020
    detail.hit.zdb_id: 207232-4
    detail.hit.zdb_id: 2016084-7
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  • 10
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    Online Resource
    The Intricate Role of Cold Gas and Dust in Galaxy Evolution at Early Cosmic Epochs
    Cambridge University Press (CUP) ; 2015
    In:  Proceedings of the International Astronomical Union Vol. 11, No. S319 ( 2015-08), p. 105-108
    Details
    In: Proceedings of the International Astronomical Union, Cambridge University Press (CUP), Vol. 11, No. S319 ( 2015-08), p. 105-108
    Abstract: Cold molecular and atomic gas plays a central role in our understanding of early galaxy formation and evolution. It represents the component of the interstellar medium (ISM) that stars form out of, and its mass, distribution, excitation, and dynamics provide crucial insight into the physical processes that support the ongoing star formation and stellar mass buildup. We here present results that demonstrate the capability of the Atacama Large (sub-)Millimeter Array (ALMA) to detect the cold ISM and dust in “normal” galaxies at redshifts z =5–6. We also show detailed studies of the ISM in massive, dust-obscured starburst galaxies out to z 〉 6 with ALMA, the Combined Array for Research in Millimeter-wave Astronomy (CARMA), the Plateau de Bure Interferometer (PdBI), and the Karl G. Jansky Very Large Array (VLA). These observations place some of the most direct constraints on the dust-obscured fraction of the star formation history of the universe at z 〉 5 to date, showing that “typical” galaxies at these epochs have low dust content, but also that highly-enriched, dusty starbursts already exist within the first billion years after the Big Bang.
    Type of Medium: Online Resource
    ISSN: 1743-9213 , 1743-9221
    URL: Article
    DOI: 10.1017/S1743921315010315
    Language: English
    Publisher: Cambridge University Press (CUP)
    Publication Date: 2015
    detail.hit.zdb_id: 2170724-8
    detail.hit.zdb_id: 232923-2
    SSG: 16,12
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