Author: "Messias H." / Publication Year Range: Last 3 years - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Messias H."' showing total 41 results

Start Over Author "Messias H." Publication Year Range Last 3 years

41 results on '"Messias H."'

1. A dusty proto-cluster surrounding the binary galaxy HerBS-70 at $z = 2.3$

Author: Bakx, Tom J. L. C., Berta, S., Dannerbauer, H., Cox, P., Butler, K. M., Hagimoto, M., Hughes, D. H., Riechers, D. A., van der Werf, P. P., Yang, C., Baker, A. J., Beelen, A., Bendo, G. J., Borsato, E., Buat, V., Cooray, A. R., Dunne, L., Dye, S., Eales, S., Gavazzi, R., Harris, A. I., Ismail, D., Ivison, R. J., Jones, B., Krips, M., Lehnert, M. D., Marchetti, L., Messias, H., Negrello, M., Neri, R., Omont, A., Perez-Fournon, I., Nanni, A., Chartab, N., Serjeant, S., Stanley, F., Tamura, Y., Urquhart, S. A., Vlahakis, C., Weiß, A., and Young, A. J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report on deep SCUBA-2 observations at 850$\mu$m and NOEMA spectroscopic measurements at 2 mm of the environment surrounding the luminous, massive ($M_{*} \approx 2 \times 10^{11}$ M$_{\odot}$) Herschel-selected source HerBS-70. This source was revealed by previous NOEMA observations to be a binary system of dusty star-forming galaxies at $z= 2.3$, with the East component (HerBS-70E) hosting an Active Galactic Nucleus (AGN). The SCUBA-2 observations detected, in addition to the binary system, twenty-one sources at $> 3.5 \sigma$ over an area of $\sim 25$ square comoving Mpc with a sensitivity of $\sigma_{850} = 0.75$ mJy. The surface density of continuum sources around HerBS-70 is three times higher than for field galaxies. The NOEMA spectroscopic measurements confirm the protocluster membership of three of the nine brightest sources through their CO(4 - 3) line emission, yielding a volume density 36 times higher than for field galaxies. All five confirmed sub-mm galaxies in the HerBS-70 system have relatively short gas depletion times ($80 - 500$ Myr), indicating the onset of quenching for this protocluster core due to the depletion of gas. The dark matter halo mass of the HerBS-70 system is estimated around $5 \times{} 10^{13}$ M$_{\odot}$, with a projected current-day mass of $10^{15}$ M$_{\odot}$, similar to the local Virgo and Coma clusters. These observations support the claim that DSFGs, in particular the ones with observed multiplicity, can trace cosmic overdensities., Comment: 19 pages, 13 figures, accepted for publication in MNRAS
Published: 2024

2. Selection of powerful radio galaxies with machine learning

Author: Carvajal, R., Matute, I., Afonso, J., Norris, R. P., Luken, K. J., Sánchez-Sáez, P., Cunha, P. A. C., Humphrey, A., Messias, H., Amarantidis, S., Barbosa, D., Cruz, H. A., Miranda, H., Paulino-Afonso, A., and Pappalardo, C.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We developed and trained a pipeline of three machine learning (ML) models than can predict which sources are more likely to be an AGN and to be detected in specific radio surveys. Also, it can estimate redshift values for predicted radio-detectable AGNs. These models, which combine predictions from tree-based and gradient-boosting algorithms, have been trained with multi-wavelength data from near-infrared-selected sources in the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) Spring field. Training, testing, calibration, and validation were carried out in the HETDEX field. Further validation was performed on near-infrared-selected sources in the Stripe 82 field. In the HETDEX validation subset, our pipeline recovers 96% of the initially labelled AGNs and, from AGNs candidates, we recover 50% of previously detected radio sources. For Stripe 82, these numbers are 94% and 55%. Compared to random selection, these rates are two and four times better for HETDEX, and 1.2 and 12 times better for Stripe 82. The pipeline can also recover the redshift distribution of these sources with $\sigma_{\mathrm{NMAD}}$ = 0.07 for HETDEX ($\sigma_{\mathrm{NMAD}}$ = 0.09 for Stripe 82) and an outlier fraction of 19% (25% for Stripe 82), compatible with previous results based on broad-band photometry. Feature importance analysis stresses the relevance of near- and mid-infrared colours to select AGNs and identify their radio and redshift nature. Combining different algorithms in ML models shows an improvement in the prediction power of our pipeline over a random selection of sources. Tree-based ML models (in contrast to deep learning techniques) facilitate the analysis of the impact that features have on the predictions. This prediction can give insight into the potential physical interplay between the properties of radio AGNs (e.g. mass of black hole and accretion rate)., Comment: Accepted for publication in A&A, 24 pages and 21 figures. Updated to include information on retrieval of data and models, which can be obtained from https://zenodo.org/doi/10.5281/zenodo.10220008
Published: 2023
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3. z-GAL -- A NOEMA spectroscopic redshift survey of bright Herschel galaxies: [III] Physical properties

Author: Berta, S., Stanley, F., Ismail, D., Cox, P., Neri, R., Yang, C., Young, A. J., Jin, S., Dannerbauer, H., Bakx, T. J., Beelen, A., Weiss, A., Nanni, A., Omont, A., van der Werf, P., Krips, M., Baker, A. J., Bendo, G., Borsato, E., Buat, V., Butler, K. M., Chartab, N., Cooray, A., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R. J., Jones, B. M., Lehnert, M., Marchetti, L., Messias, H., Negrello, M., Perez-Fournon, I., Riechers, D. A., Serjeant, S., Urquhart, S., and Vlahakis, C.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The z-GAL survey observed 137 bright Herschel-selected targets with the IRAM NOrthern Extended Millimeter Array, with the aim to measure their redshift and study their properties. Several of them have been resolved into multiple sources. Consequently, robust spectroscopic redshifts have been measured for 165 individual galaxies in the range 0.8
Published: 2023
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4. z-GAL -- A NOEMA spectroscopic redshift survey of bright Herschel galaxies: [II] Dust properties

Author: Ismail, D., Beelen, A., Buat, V., Berta, S., Cox, P., Stanley, F., Young, A., Jin, S., Neri, R., Bakx, T., Dannerbauer, H., Butler, K., Cooray, A., Nanni, A., Omont, A., Serjeant, S., van der Werf, P., Vlahakis, C., Weiss, A., Yang, C., Baker, A. J., Bendo, G., Borsato, E., Chartab, N., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R., Krips, B. M. Jones M., Lehnert, M., Marchetti, L., Messias, H., Negrello, M., Perez-Fournon, I., Riechers, D. A., and Urquhart, S.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: (Abridged) We present the dust properties of 125 bright Herschel galaxies selected from the z-GAL survey. The large instantaneous bandwidth of NOEMA provides an exquisite sampling of the underlying dust continuum emission at 2 and 3 mm in the observed frame, with flux densities in at least four side bands for each source. Together with the available Herschel 250, 350, and 500 micron and SCUBA-2 850 micron flux densities, the spectral energy distribution of each source can be analyzed from the far-infrared to the millimeter, with a fine sampling of the Rayleigh-Jeans tail. This wealth of data provides a solid basis to derive robust dust properties, in particular the dust emissivity index, beta, and the dust temperature, T(dust). In order to demonstrate our ability to constrain the dust properties, we used a flux-generated mock catalog and analyzed the results under the assumption of an optically thin and optically thick modified black body emission. For the z-GAL sources, we report a range of dust emissivities with beta ~ 1.5 - 3 estimated up to high precision with relative uncertainties that vary in the range 7% - 15%, and an average of 2.2 +/- 0.3. We find dust temperatures varying from 20 to 50 K with an average of T(dust) ~ 30 K for the optically thin case and ~38 K in the optically thick case. For all the sources, we estimate the dust masses and apparent infrared luminosities (based on the optically thin approach). An inverse correlation is found between T(dust) and beta, which is similar to what is seen in the local Universe. Finally, we report an increasing trend in the dust temperature as a function of redshift at a rate of 6.5 +/- 0.5 K/z for this 500 micron-selected sample. Based on this study, future prospects are outlined to further explore the evolution of dust temperature across cosmic time., Comment: Accepted for publication on A&A; 32 pages; 26 figures
Published: 2023
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5. z-GAL -- A NOEMA spectroscopic redshift survey of bright Herschel galaxies: [I] Overview

Author: Cox, P., Neri, R., Berta, S., Ismail, D., Stanley, F., Young, A., Jin, S., Bakx, T., Beelen, A., Dannerbauer, H., Krips, M., Lehnert, M., Omont, A., Riechers, D. A., Baker, A. J., Bendo, G., Borsato, E., Buat, V., Butler, K., Chartab, N., Cooray, A., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R., Jones, B. M., Marchetti, L., Messias, H., Nanni, A., Negrello, M., Perez-Fournon, I., Serjeant, S., Urquhart, S., Vlahakis, C., Weiss, A., van der Werf, P., and Yang, C.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: (Abridged) Using the IRAM NOEMA interferometer, we measures the redshifts of 126 bright galaxies detected in the Herschel H-ATLAS, HeLMS, and HerS surveys. We report reliable spectroscopic redshifts for a total of 124 of the Herschel-selected galaxies. The redshifts are estimated from scans of the 3 and 2-mm bands (and, in one case, the 1-mm band) and are based on the detection of at least two emission lines. Together with the Pilot Programme (Neri et al. 2020), including spectroscopic redshifts of 11 sources, our survey has derived precise redshifts for 135 bright Herschel-selected galaxies, making it the largest sample of high-z galaxies with robust redshifts to date. Most emission lines detected are from 12CO (mainly from J=2-1 to 5-4), with some sources seen in [CI] and H2O emission lines. The spectroscopic redshifts are in the range 0.8
Published: 2023
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6. ALMA High-Level Data Products: Submillimetre counterparts of SDSS quasars in the ALMA footprint

Author: Wong, A., Hatziminaoglou, E., Borkar, A., Popping, G., Pérez-Fournon, I., Poidevin, F., Stoehr, F., and Messias, H.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The Atacama Large Millimetre/submillimetre Array (ALMA) is the world's most advanced radio interferometric facility, producing science data with an average rate of about 1 TB per day. After a process of calibration, imaging and quality assurance, the scientific data are stored in the ALMA Science Archive (ASA), along with the corresponding raw data, making the ASA an invaluable resource for original astronomical research. Due to their complexity, each ALMA data set has the potential for scientific results that go well beyond the ideas behind the original proposal that led to each observation. For this reason, the European ALMA Regional Centre initiated the High-Level Data Products initiative to develop science-oriented data products derived from data sets publicly available in the ASA, that go beyond the formal ALMA deliverables. The first instance of this initiative is the creation of a catalogue of submillimetre (submm) detections of Sloan Digital Sky Survey (SDSS) quasars from the SDSS Data Release 14 that lie in the aggregate ALMA footprint observed since ALMA Cycle 0. The ALMA fluxes are extracted in an automatic fashion, using the ALMA Data Mining Toolkit. All extractions above a signal-to-noise cut of 3.5 are considered, they have been visually inspected and the reliable detections are presented in a catalogue of 376 entries, corresponding to 275 unique quasars. Interesting targets found in the process, i.e. lensed or jetted quasars as well as quasars with nearby submm counterparts are highlighted, to facilitate further studies or potential follow up observations.
Published: 2023
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7. Bright Extragalactic ALMA Redshift Survey (BEARS) III: Detailed study of emission lines from 71 Herschel targets

Author: Hagimoto, M., Bakx, T. J. L. C., Serjeant, S., Bendo, G. J., Urquhart, S. A., Eales, S., Harrington, K. C., Tamura, Y., Umehata, H., Berta, S., Cooray, A. R., Cox, P., De Zotti, G., Lehnert, M. D., Riechers, D. A., Scott, D., Temi, P., van der Werf, P. P., Yang, C., Amvrosiadis, A., Andreani, P. M., Baker, A. J., Beelen, A., Borsato, E., Buat, V., Butler, K. M., Dannerbauer, H., Dunne, L., Dye, S., Enia, A. F. M., Fan, L., Gavazzi, R., Gonzalez-Nuevo, J., Harris, A. I., Herrera, C. N., Hughes, D. H., Ismail, D., Ivison, R. J., Jones, B., Kohno, K., Krips, M., Lagache, G., Marchetti, L., Massardi, M., Messias, H., Negrello, M., Neri, R., Omont, A., Perez-Fournon, I., Sedgwick, C., Smith, M. W. L., Stanley, F., Verma, A., Vlahakis, C., Ward, B., Weiner, C., Weiss, A., and Young, A. J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We analyse the molecular and atomic emission lines of 71 bright Herschel-selected galaxies between redshifts 1.4 to 4.6 detected by the Atacama Large Millimetre/submillimetre Array. These lines include a total of 156 CO, [C I], and H2O emission lines. For 46 galaxies, we detect two transitions of CO lines, and for these galaxies we find gas properties similar to those of other dusty star-forming galaxy (DSFG) samples. A comparison to photo-dissociation models suggests that most of Herschel-selected galaxies have similar interstellar medium conditions as local infrared-luminous galaxies and high-redshift DSFGs, although with denser gas and more intense far-ultraviolet radiation fields than normal star-forming galaxies. The line luminosities agree with the luminosity scaling relations across five orders of magnitude, although the star-formation and gas surface density distributions (i.e., Schmidt-Kennicutt relation) suggest a different star-formation phase in our galaxies (and other DSFGs) compared to local and low-redshift gas-rich, normal star-forming systems. The gas-to-dust ratios of these galaxies are similar to Milky Way values, with no apparent redshift evolution. Four of 46 sources appear to have CO line ratios in excess of the expected maximum (thermalized) profile, suggesting a rare phase in the evolution of DSFGs. Finally, we create a deep stacked spectrum over a wide rest-frame frequency (220-890 GHz) that reveals faint transitions from HCN and CH, in line with previous stacking experiments., Comment: 30 pages, 17 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society Main Journal. Comments are warmly welcomed
Published: 2023
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8. The Bright Extragalactic ALMA Redshift Survey (BEARS) II: Millimetre photometry of gravitational lens candidates

Author: Bendo, G. J., Urquhart, S. A., Serjeant, S., Bakx, T., Hagimoto, M., Cox, P., Neri, R., Lehnert, M. D., Dannerbauer, H., Amvrosiadis, A., Andreani, P., Baker, A. J., Beelen, A., Berta, S., Borsato, E., Buat, V., Butler, K. M., Cooray, A., De Zotti, G., Dunne, L., Dye, S., Eales, S., Enia, A., Fan, L., Gavazzi, R., González-Nuevo, J., Harris, A. I., Herrera, C. N., Hughes, D. H., Ismail, D., Jones, B. M., Kohno, K., Krips, M., Lagache, G., Marchetti, L., Massardi, M., Messias, H., Negrello, M., Omont, A., Pérez-Fournon, I., Riechers, D. A., Scott, D., Smith, M. W. L., Stanley, F., Tamura, Y., Temi, P., van der Werf, P., Verma, A., Vlahakis, C., Weiß, A., Yang, C., and Young, A. J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present 101 and 151 GHz ALMA continuum images for 85 fields selected from Herschel observations that have 500 micron flux densities >80 mJy and 250-500 micron colours consistent with z > 2, most of which are expected to be gravitationally lensed or hyperluminous infrared galaxies. Approximately half of the Herschel 500 micron sources were resolved into multiple ALMA sources, but 11 of the 15 brightest 500 micron Herschel sources correspond to individual ALMA sources. For the 37 fields containing either a single source with a spectroscopic redshift or two sources with the same spectroscopic redshift, we examined the colour temperatures and dust emissivity indices. The colour temperatures only vary weakly with redshift and are statistically consistent with no redshift-dependent temperature variations, which generally corresponds to results from other samples selected in far-infrared, submillimetre, or millimetre bands but not to results from samples selected in optical or near-infrared bands. The dust emissivity indices, with very few exceptions, are largely consistent with a value of 2. We also compared spectroscopic redshifts to photometric redshifts based on spectral energy distribution templates designed for infrared-bright high-redshift galaxies. While the templates systematically underestimate the redshifts by ~15%, the inclusion of ALMA data decreases the scatter in the predicted redshifts by a factor of ~2, illustrating the potential usefulness of these millimetre data for estimating photometric redshifts., Comment: Accepted for publication in Monthly Notices of the Royal Astronomical Society
Published: 2023
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9. The Bright Extragalactic ALMA Redshift Survey (BEARS) I: redshifts of bright gravitationally-lensed galaxies from the Herschel ATLAS

Author: Urquhart, S. A., Bendo, G. J., Serjeant, S., Bakx, T., Hagimoto, M., Cox, P., Neri, R., Lehnert, M., Sedgwick, C., Weiner, C., Dannerbauer, H., Amvrosiadis, A., Andreani, P., Baker, A. J., Beelen, A., Berta, S., Borsato, E., Buat, V., Butler, K. M., Cooray, A., De Zotti, G., Dunne, L., Dye, S., Eales, S., Enia, A., Fan, L., Gavazzi, R., Gonzalez-Nuevo, J., Harris, A. I., Herrera, C. N., Hughes, D., Ismail, D., Ivison, R., Jin, S., Jones, B., Kohno, K., Krips, M., Lagache, G., Marchetti, L., Massardi, M., Messias, H., Negrello, M., Omont, A., Perez-Fournon, I., Riechers, D. A., Scott, D., Smith, M. W. L., Stanley, F., Tamura, Y., Temi, P., Vlahakis, C., Weiss, A., van der Werf, P., Verma, A., Yang, C., and Young, A. J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present spectroscopic measurements for 71 galaxies associated with 62 of the brightest high-redshift submillimeter sources from the Southern fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), while targeting 85 sources which resolved into 142. We have obtained robust redshift measurements for all sources using the 12-m Array and an efficient tuning of ALMA to optimise its use as a redshift hunter, with 73 per cent of the sources having a robust redshift identification. Nine of these redshift identifications also rely on observations from the Atacama Compact Array. The spectroscopic redshifts span a range $1.41
Published: 2022
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10. A dusty proto-cluster surrounding the binary galaxy HerBS-70 at z = 2.3

Author: Bakx, Tom J L C, primary, Berta, S, additional, Dannerbauer, H, additional, Cox, P, additional, Butler, K M, additional, Hagimoto, M, additional, Hughes, D H, additional, Riechers, D A, additional, van der Werf, P P, additional, Yang, C, additional, Baker, A J, additional, Beelen, A, additional, Bendo, G J, additional, Borsato, E, additional, Buat, V, additional, Cooray, A R, additional, Dunne, L, additional, Dye, S, additional, Eales, S, additional, Gavazzi, R, additional, Harris, A I, additional, Ismail, D, additional, Ivison, R J, additional, Jones, B, additional, Krips, M, additional, Lehnert, M D, additional, Marchetti, L, additional, Messias, H, additional, Negrello, M, additional, Neri, R, additional, Omont, A, additional, Perez-Fournon, I, additional, Nanni, A, additional, Chartab, N, additional, Serjeant, S, additional, Stanley, F, additional, Tamura, Y, additional, Urquhart, S A, additional, Vlahakis, C, additional, Weiß, A, additional, and Young, A J, additional
Published: 2024
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11. z-GAL: A NOEMA spectroscopic redshift survey of bright Herschel galaxies

Author: Cox, P., primary, Neri, R., additional, Berta, S., additional, Ismail, D., additional, Stanley, F., additional, Young, A., additional, Jin, S., additional, Bakx, T., additional, Beelen, A., additional, Dannerbauer, H., additional, Krips, M., additional, Lehnert, M., additional, Omont, A., additional, Riechers, D. A., additional, Baker, A. J., additional, Bendo, G., additional, Borsato, E., additional, Buat, V., additional, Butler, K., additional, Chartab, N., additional, Cooray, A., additional, Dye, S., additional, Eales, S., additional, Gavazzi, R., additional, Hughes, D., additional, Ivison, R., additional, Jones, B. M., additional, Marchetti, L., additional, Messias, H., additional, Nanni, A., additional, Negrello, M., additional, Perez-Fournon, I., additional, Serjeant, S., additional, Urquhart, S., additional, Vlahakis, C., additional, Weiß, A., additional, van der Werf, P., additional, and Yang, C., additional
Published: 2024
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12. z-GAL: A NOEMA spectroscopic redshift survey of brightHerschelgalaxies

Author: Cox, P., primary, Neri, R., additional, Berta, S., additional, Ismail, D., additional, Stanley, F., additional, Young, A., additional, Jin, S., additional, Bakx, T., additional, Beelen, A., additional, Dannerbauer, H., additional, Krips, M., additional, Lehnert, M., additional, Omont, A., additional, Riechers, D. A., additional, Baker, A. J., additional, Bendo, G., additional, Borsato, E., additional, Buat, V., additional, Butler, K., additional, Chartab, N., additional, Cooray, A., additional, Dye, S., additional, Eales, S., additional, Gavazzi, R., additional, Hughes, D., additional, Ivison, R., additional, Jones, B. M., additional, Marchetti, L., additional, Messias, H., additional, Nanni, A., additional, Negrello, M., additional, Perez-Fournon, I., additional, Serjeant, S., additional, Urquhart, S., additional, Vlahakis, C., additional, Weiß, A., additional, van der Werf, P., additional, and Yang, C., additional
Published: 2023
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13. z-GAL: A NOEMA spectroscopic redshift survey of brightHerschelgalaxies

Author: Ismail, D., primary, Beelen, A., additional, Buat, V., additional, Berta, S., additional, Cox, P., additional, Stanley, F., additional, Young, A., additional, Jin, S., additional, Neri, R., additional, Bakx, T., additional, Dannerbauer, H., additional, Butler, K., additional, Cooray, A., additional, Nanni, A., additional, Omont, A., additional, Serjeant, S., additional, van der Werf, P., additional, Vlahakis, C., additional, Weiß, A., additional, Yang, C., additional, Baker, A. J., additional, Bendo, G., additional, Borsato, E., additional, Chartab, N., additional, Dye, S., additional, Eales, S., additional, Gavazzi, R., additional, Hughes, D., additional, Ivison, R., additional, Jones, B. M., additional, Krips, M., additional, Lehnert, M., additional, Marchetti, L., additional, Messias, H., additional, Negrello, M., additional, Perez-Fournon, I., additional, Riechers, D. A., additional, and Urquhart, S., additional
Published: 2023
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14. z-GAL: A NOEMA spectroscopic redshift survey of bright Herschel galaxies

Author: Berta, S., primary, Stanley, F., additional, Ismail, D., additional, Cox, P., additional, Neri, R., additional, Yang, C., additional, Young, A. J., additional, Jin, S., additional, Dannerbauer, H., additional, Bakx, T. J. L. C., additional, Beelen, A., additional, Weiß, A., additional, Nanni, A., additional, Omont, A., additional, van der Werf, P., additional, Krips, M., additional, Baker, A. J., additional, Bendo, G., additional, Borsato, E., additional, Buat, V., additional, Butler, K. M., additional, Chartab, N., additional, Cooray, A., additional, Dye, S., additional, Eales, S., additional, Gavazzi, R., additional, Hughes, D., additional, Ivison, R. J., additional, Jones, B. M., additional, Lehnert, M., additional, Marchetti, L., additional, Messias, H., additional, Negrello, M., additional, Perez-Fournon, I., additional, Riechers, D. A., additional, Serjeant, S., additional, Urquhart, S., additional, and Vlahakis, C., additional
Published: 2023
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15. Selection of powerful radio galaxies with machine learning

Author: Carvajal, R., primary, Matute, I., additional, Afonso, J., additional, Norris, R. P., additional, Luken, K. J., additional, Sánchez-Sáez, P., additional, Cunha, P., additional, Humphrey, A., additional, Messias, H., additional, Amarantidis, S., additional, Barbosa, D., additional, Cruz, H. A., additional, Miranda, H., additional, Paulino-Afonso, A., additional, and Pappalardo, C., additional
Published: 2023
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16. Tracing obscured galaxy build-up at high redshift using deep radio surveys

Author: Amarantidis, S., primary, Afonso, J., additional, Matute, I., additional, Farrah, D., additional, Hopkins, A. M., additional, Messias, H., additional, Pappalardo, C., additional, and Seymour, N., additional
Published: 2023
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17. ALMA High-Level Data Products: Submillimetre counterparts of SDSS quasars in the ALMA footprint

Author: Wong, A, primary, Hatziminaoglou, E, additional, Borkar, A, additional, Popping, G, additional, Pérez-Fournon, I, additional, Poidevin, F, additional, Stoehr, F, additional, and Messias, H, additional
Published: 2023
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18. z-GAL:A NOEMA spectroscopic redshift survey of bright Herschel galaxies: I. Overview

Author: Cox, P., Neri, R., Berta, S., Ismail, D., Stanley, F., Young, A., Jin, S., Bakx, T., Beelen, A., Dannerbauer, H., Krips, M., Lehnert, M., Omont, A., Riechers, D. A., Baker, A. J., Bendo, G., Borsato, E., Buat, V., Butler, K., Chartab, N., Cooray, A., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R., Jones, B. M., Marchetti, L., Messias, H., Nanni, A., Negrello, M., Perez-Fournon, I., Serjeant, S., Urquhart, S., Vlahakis, C., Weiab, A., Van Der Werf, P., Yang, C., Cox, P., Neri, R., Berta, S., Ismail, D., Stanley, F., Young, A., Jin, S., Bakx, T., Beelen, A., Dannerbauer, H., Krips, M., Lehnert, M., Omont, A., Riechers, D. A., Baker, A. J., Bendo, G., Borsato, E., Buat, V., Butler, K., Chartab, N., Cooray, A., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R., Jones, B. M., Marchetti, L., Messias, H., Nanni, A., Negrello, M., Perez-Fournon, I., Serjeant, S., Urquhart, S., Vlahakis, C., Weiab, A., Van Der Werf, P., and Yang, C.
Abstract: Using the IRAM NOrthern Extended Millimetre Array (NOEMA), we conducted a Large Programme (z-GAL) to measure redshifts for 126 bright galaxies detected in the Herschel Astrophysical Large Area Survey (H-ATLAS), the HerMES Large Mode Survey (HeLMS), and the Herschel Stripe 82 (HerS) Survey. We report reliable spectroscopic redshifts for a total of 124 of the Herschel-selected galaxies. The redshifts are estimated from scans of the 3 and 2-mm bands (and, for one source, the 1-mm band), covering up to 31 GHz in each band, and are based on the detection of at least two emission lines. Together with the Pilot Programme, where 11 sources had their spectroscopic redshifts measured, our survey has derived precise redshifts for 135 bright Herschel-selected galaxies, making it the largest sample of high-z galaxies with robust redshifts to date. Most emission lines detected are from 12CO (mainly from J = 2 1 to 5 4), with some sources seen in [CI] and H2O emission lines. The spectroscopic redshifts are in the range 0.8 < z < 6.55 with a median value of z = 2.56 ± 0.10, centred on the peak epoch of galaxy formation. The linewidths of the sources are large, with a mean value for the full width at half maximum I- V of 590 ± 25 km s-1 and with 35% of the sources having widths of 700 km s-1 < I- V < 1800 km s-1. Most of the sources are unresolved or barely resolved on scales of ∼2 to 3; (or linear sizes of ∼15 - 25 kpc, unlensed). Some fields reveal double or multiple sources in line emission and the underlying dust continuum and, in some cases, sources at different redshifts. Taking these sources into account, there are, in total, 165 individual sources with robust spectroscopic redshifts, including lensed galaxies, binary systems, and over-densities. This paper presents an overview of the z-GAL survey and provides the observed properties of the emission lines, the derived spectroscopic redshifts, and a catalogu
Published: 2023

19. z -GAL:A NOEMA spectroscopic redshift survey of bright Herschel galaxies: III. Physical properties

Author: Berta, S., Stanley, F., Ismail, D., Cox, P., Neri, R., Yang, C., Young, A. J., Jin, S., Dannerbauer, H., Bakx, T. J.L.C., Beelen, A., Weib, A., Nanni, A., Omont, A., Van Der Werf, P., Krips, M., Baker, A. J., Bendo, G., Borsato, E., Buat, V., Butler, K. M., Chartab, N., Cooray, A., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R. J., Jones, B. M., Lehnert, M., Marchetti, L., Messias, H., Negrello, M., Perez-Fournon, I., Riechers, D. A., Serjeant, S., Urquhart, S., Vlahakis, C., Berta, S., Stanley, F., Ismail, D., Cox, P., Neri, R., Yang, C., Young, A. J., Jin, S., Dannerbauer, H., Bakx, T. J.L.C., Beelen, A., Weib, A., Nanni, A., Omont, A., Van Der Werf, P., Krips, M., Baker, A. J., Bendo, G., Borsato, E., Buat, V., Butler, K. M., Chartab, N., Cooray, A., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R. J., Jones, B. M., Lehnert, M., Marchetti, L., Messias, H., Negrello, M., Perez-Fournon, I., Riechers, D. A., Serjeant, S., Urquhart, S., and Vlahakis, C.
Abstract: The z-GAL survey observed 137 bright Herschel-selected targets with the IRAM Northern Extended Millimeter Array, with the aim to measure their redshift and study their properties. Several of them have been resolved into multiple sources. Consequently, robust spectroscopic redshifts have been measured for 165 individual galaxies in the range 0.8., <., z., <., 6.5. In this paper we analyse the millimetre spectra of the z-GAL sources, using both their continuum and line emission to derive their physical properties. At least two spectral lines are detected for each source, including transitions of 12CO, [CI], and H2O. The observed 12CO line ratios and spectral line energy distributions of individual sources resemble those of local starbursts. In seven sources the para-H2O (211-202) transition is detected and follows the IR versus H2O luminosity relation of sub-millimetre galaxies. The molecular gas mass of the z-GAL sources is derived from their 12CO, [CI], and sub-millimetre dust continuum emission. The three tracers lead to consistent results, with the dust continuum showing the largest scatter when compared to 12CO. The gas-to-dust mass ratio of these sources was computed by combining the information derived from 12CO and the dust continuum and has a median value of 107, similar to star-forming galaxies of near-solar metallicity. The same combined analysis leads to depletion timescales in the range between 0.1 and 1.0 Gyr, which place the z-GAL sources between the main sequence' of star formation and the locus of starbursts. Finally, we derived a first estimate of stellar masses "modulo possible gravitational magnification "by inverting known gas scaling relations: the z-GAL sample is confirmed to be mostly composed by starbursts, whereas ∼25% of its members lie on the main sequence of star-forming galaxies (within ±0.5 dex).
Published: 2023

20. The hidden side of cosmic star formation at z > 3 Bridging optically dark and Lyman-break galaxies with GOODS-ALMA

Author: Xiao, M.-y., Elbaz, D., Gómez-guijarro, C., Leroy, L., Bing, L.-j., Daddi, E., Magnelli, B., Franco, M., Zhou, L., Dickinson, M., Wang, T., Rujopakarn, W., Magdis, G. E., Treister, E., Inami, H., Demarco, R., Sargent, M. T., Shu, X., Kartaltepe, J. S., Alexander, D. M., Béthermin, M., Bournaud, F., Ciesla, L., Ferguson, H. C., Finkelstein, S. L., Giavalisco, M., Gu, Q.-s., Iono, D., Juneau, S., Lagache, G., Leiton, R., Messias, H., Motohara, K., Mullaney, J., Nagar, N., Pannella, M., Papovich, C., Pope, A., Schreiber, C., Silverman, J., Xiao, M.-y., Elbaz, D., Gómez-guijarro, C., Leroy, L., Bing, L.-j., Daddi, E., Magnelli, B., Franco, M., Zhou, L., Dickinson, M., Wang, T., Rujopakarn, W., Magdis, G. E., Treister, E., Inami, H., Demarco, R., Sargent, M. T., Shu, X., Kartaltepe, J. S., Alexander, D. M., Béthermin, M., Bournaud, F., Ciesla, L., Ferguson, H. C., Finkelstein, S. L., Giavalisco, M., Gu, Q.-s., Iono, D., Juneau, S., Lagache, G., Leiton, R., Messias, H., Motohara, K., Mullaney, J., Nagar, N., Pannella, M., Papovich, C., Pope, A., Schreiber, C., and Silverman, J.
Published: 2023

21. The hidden side of cosmic star formation at z > 3:Bridging optically dark and Lyman-break galaxies with GOODS-ALMA

Author: Xiao, M. Y., Elbaz, D., Gómez-Guijarro, C., Leroy, L., Bing, L. J., Daddi, E., Magnelli, B., Franco, M., Zhou, L., Dickinson, M., Wang, T., Rujopakarn, W., Magdis, G. E., Treister, E., Inami, H., Demarco, R., Sargent, M. T., Shu, X., Kartaltepe, J. S., Alexander, D. M., Béthermin, M., Bournaud, F., Ciesla, L., Ferguson, H. C., Finkelstein, S. L., Giavalisco, M., Gu, Q. S., Iono, D., Juneau, S., Lagache, G., Leiton, R., Messias, H., Motohara, K., Mullaney, J., Nagar, N., Pannella, M., Papovich, C., Pope, A., Schreiber, C., Silverman, J., Xiao, M. Y., Elbaz, D., Gómez-Guijarro, C., Leroy, L., Bing, L. J., Daddi, E., Magnelli, B., Franco, M., Zhou, L., Dickinson, M., Wang, T., Rujopakarn, W., Magdis, G. E., Treister, E., Inami, H., Demarco, R., Sargent, M. T., Shu, X., Kartaltepe, J. S., Alexander, D. M., Béthermin, M., Bournaud, F., Ciesla, L., Ferguson, H. C., Finkelstein, S. L., Giavalisco, M., Gu, Q. S., Iono, D., Juneau, S., Lagache, G., Leiton, R., Messias, H., Motohara, K., Mullaney, J., Nagar, N., Pannella, M., Papovich, C., Pope, A., Schreiber, C., and Silverman, J.
Abstract: Our current understanding of the cosmic star formation history at z > 3 is primarily based on UV-selected galaxies (Lyman-break galaxies, i.e., LBGs). Recent studies of H-dropouts (HST-dark galaxies) have revealed that we may be missing a large proportion of star formation that is taking place in massive galaxies at z > 3. In this work, we extend the H-dropout criterion to lower masses to select optically dark or faint galaxies (OFGs) at high redshifts in order to complete the census between LBGs and H-dropouts. Our criterion (H > 26.5 mag & [4.5] < 25 mag) combined with a de-blending technique is designed to select not only extremely dust-obscured massive galaxies but also normal star-forming galaxies (typically E(B − V) > 0.4) with lower stellar masses at high redshifts. In addition, with this criterion, our sample is not contaminated by massive passive or old galaxies. In total, we identified 27 OFGs at zphot > 3 (with a median of zmed = 4.1) in the GOODS-ALMA field, covering a wide distribution of stellar masses with log(M⋆/M⊙) = 9.4 − 11.1 (with a median of log(M⋆med/M⊙) = 10.3). We find that up to 75% of the OFGs with log(M⋆/M⊙) = 9.5 − 10.5 were neglected by previous LBGs and H-dropout selection techniques. After performing an optical-to-millimeter stacking analysis of the OFGs, we find that rather than being limited to a rare population of extreme starbursts, these OFGs represent a normal population of dusty star-forming galaxies at z > 3. The OFGs exhibit shorter gas depletion timescales, slightly lower gas fractions, and lower dust temperatures than the scaling relation of typical star-forming galaxies. Additionally, the total star formation rate (SFRtot = SFRIR + SFRUV) of the stac
Published: 2023

22. z-GAL:A NOEMA spectroscopic redshift survey of bright Herschel galaxies: I.Overview

Author: Cox, P., Neri, R., Berta, S., Ismail, D., Stanley, F., Young, A., Jin, S., Bakx, T., Beelen, A., Dannerbauer, H., Krips, M., Lehnert, M., Omont, A., Riechers, D. A., Baker, A. J., Bendo, G., Borsato, E., Buat, V., Butler, K., Chartab, N., Cooray, A., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R., Jones, B. M., Marchetti, L., Messias, H., Nanni, A., Negrello, M., Perez-fournon, I., Serjeant, S., Urquhart, S., Vlahakis, C., Weiß, A., Van Der Werf, P., Yang, C., Cox, P., Neri, R., Berta, S., Ismail, D., Stanley, F., Young, A., Jin, S., Bakx, T., Beelen, A., Dannerbauer, H., Krips, M., Lehnert, M., Omont, A., Riechers, D. A., Baker, A. J., Bendo, G., Borsato, E., Buat, V., Butler, K., Chartab, N., Cooray, A., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R., Jones, B. M., Marchetti, L., Messias, H., Nanni, A., Negrello, M., Perez-fournon, I., Serjeant, S., Urquhart, S., Vlahakis, C., Weiß, A., Van Der Werf, P., and Yang, C.
Published: 2023

23. z -GAL:A NOEMA spectroscopic redshift survey of bright Herschel galaxies II. Dust properties

Author: Ismail, D., Beelen, A., Buat, V., Berta, S., Cox, P., Stanley, F., Young, A., Jin, S., Neri, R., Bakx, T., Dannerbauer, H., Butler, K., Cooray, A., Nanni, A., Omont, A., Serjeant, S., Van Der Werf, P., Vlahakis, C., Weiß, A., Yang, C., Baker, A. J., Bendo, G., Borsato, E., Chartab, N., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R., Jones, B. M., Krips, M., Lehnert, M., Marchetti, L., Messias, H., Negrello, M., Perez-fournon, I., Riechers, D. A., Urquhart, S., Ismail, D., Beelen, A., Buat, V., Berta, S., Cox, P., Stanley, F., Young, A., Jin, S., Neri, R., Bakx, T., Dannerbauer, H., Butler, K., Cooray, A., Nanni, A., Omont, A., Serjeant, S., Van Der Werf, P., Vlahakis, C., Weiß, A., Yang, C., Baker, A. J., Bendo, G., Borsato, E., Chartab, N., Dye, S., Eales, S., Gavazzi, R., Hughes, D., Ivison, R., Jones, B. M., Krips, M., Lehnert, M., Marchetti, L., Messias, H., Negrello, M., Perez-fournon, I., Riechers, D. A., and Urquhart, S.
Published: 2023

24. The hidden side of cosmic star formation at z > 3

Author: Xiao, M.-Y., primary, Elbaz, D., additional, Gómez-Guijarro, C., additional, Leroy, L., additional, Bing, L.-J., additional, Daddi, E., additional, Magnelli, B., additional, Franco, M., additional, Zhou, L., additional, Dickinson, M., additional, Wang, T., additional, Rujopakarn, W., additional, Magdis, G. E., additional, Treister, E., additional, Inami, H., additional, Demarco, R., additional, Sargent, M. T., additional, Shu, X., additional, Kartaltepe, J. S., additional, Alexander, D. M., additional, Béthermin, M., additional, Bournaud, F., additional, Ciesla, L., additional, Ferguson, H. C., additional, Finkelstein, S. L., additional, Giavalisco, M., additional, Gu, Q.-S., additional, Iono, D., additional, Juneau, S., additional, Lagache, G., additional, Leiton, R., additional, Messias, H., additional, Motohara, K., additional, Mullaney, J., additional, Nagar, N., additional, Pannella, M., additional, Papovich, C., additional, Pope, A., additional, Schreiber, C., additional, and Silverman, J., additional
Published: 2023
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25. Bright extragalactic ALMA redshift survey (BEARS) III: detailed study of emission lines from 71Herscheltargets

Author: Hagimoto, M, primary, Bakx, T J L C, additional, Serjeant, S, additional, Bendo, G J, additional, Urquhart, S A, additional, Eales, S, additional, Harrington, K C, additional, Tamura, Y, additional, Umehata, H, additional, Berta, S, additional, Cooray, A R, additional, Cox, P, additional, De Zotti, G, additional, Lehnert, M D, additional, Riechers, D A, additional, Scott, D, additional, Temi, P, additional, van der Werf, P P, additional, Yang, C, additional, Amvrosiadis, A, additional, Andreani, P M, additional, Baker, A J, additional, Beelen, A, additional, Borsato, E, additional, Buat, V, additional, Butler, K M, additional, Dannerbauer, H, additional, Dunne, L, additional, Dye, S, additional, Enia, A F M, additional, Fan, L, additional, Gavazzi, R, additional, González-Nuevo, J, additional, Harris, A I, additional, Herrera, C N, additional, Hughes, D H, additional, Ismail, D, additional, Ivison, R J, additional, Jones, B, additional, Kohno, K, additional, Krips, M, additional, Lagache, G, additional, Marchetti, L, additional, Massardi, M, additional, Messias, H, additional, Negrello, M, additional, Neri, R, additional, Omont, A, additional, Perez-Fournon, I, additional, Sedgwick, C, additional, Smith, M W L, additional, Stanley, F, additional, Verma, A, additional, Vlahakis, C, additional, Ward, B, additional, Weiner, C, additional, Weiß, A, additional, and Young, A J, additional
Published: 2023
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26. Orbital motion near Sagittarius A*

Author: Wielgus, M., primary, Moscibrodzka, M., additional, Vos, J., additional, Gelles, Z., additional, Martí-Vidal, I., additional, Farah, J., additional, Marchili, N., additional, Goddi, C., additional, and Messias, H., additional
Published: 2022
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27. The bright extragalactic ALMA redshift survey (BEARS) – II. Millimetre photometry of gravitational lens candidates

Author: Bendo, G J, primary, Urquhart, S A, additional, Serjeant, S, additional, Bakx, T, additional, Hagimoto, M, additional, Cox, P, additional, Neri, R, additional, Lehnert, M D, additional, Dannerbauer, H, additional, Amvrosiadis, A, additional, Andreani, P, additional, Baker, A J, additional, Beelen, A, additional, Berta, S, additional, Borsato, E, additional, Buat, V, additional, Butler, K M, additional, Cooray, A, additional, De Zotti, G, additional, Dunne, L, additional, Dye, S, additional, Eales, S, additional, Enia, A, additional, Fan, L, additional, Gavazzi, R, additional, González-Nuevo, J, additional, Harris, A I, additional, Herrera, C N, additional, Hughes, D H, additional, Ismail, D, additional, Jones, B M, additional, Kohno, K, additional, Krips, M, additional, Lagache, G, additional, Marchetti, L, additional, Massardi, M, additional, Messias, H, additional, Negrello, M, additional, Omont, A, additional, Pérez-Fournon, I, additional, Riechers, D A, additional, Scott, D, additional, Smith, M W L, additional, Stanley, F, additional, Tamura, Y, additional, Temi, P, additional, van der Werf, P, additional, Verma, A, additional, Vlahakis, C, additional, Weiß, A, additional, Yang, C, additional, and Young, A J, additional
Published: 2022
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28. The bright extragalactic ALMA redshift survey (BEARS) I: redshifts of bright gravitationally lensed galaxies from the Herschel ATLAS

Author: Dye, S, Urquhart, S A, Bendo, G J, Serjeant, S, Bakx, T, Hagimoto, M, Cox, P, Neri, R, Lehnert, M, Sedgwick, C, Weiner, C, Dannerbauer, H, Amvrosiadis, A, Andreani, P, Baker, A J, Beelen, A, Berta, S, Borsato, E, Buat, V, Butler, K M, Cooray, A, De Zotti, G, Kohno, K, Dunne, L, Eales, S, Enia, A, Fan, L, Gavazzi, R, Harris, A I, Herrera, C N, Hughes, D, Ismail, D, Ivison, R, Jin, S, Jones, B, Krips, M, Lagache, G, Marchetti, L, Massardi, M, Messias, H, Negrello, M, Omont, A, Perez-Fournon, I, Riechers, D A, Scott, D, Smith, M W L, Stanley, F, Tamura, Y, Temi, P, Vlahakis, C, Werf, P, Verma, A, Yang, C, and Young, A J
Subjects: Space and Planetary Science, Astronomy and Astrophysics
Abstract: We present spectroscopic measurements for 71 galaxies associated with 62 of the brightest high-redshift submillimetre sources from the Southern fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), while targeting 85 sources which resolved into 142. We have obtained robust redshift measurements for all sources using the 12-m Array and an efficient tuning of ALMA to optimize its use as a redshift hunter, with 73 per cent of the sources having a robust redshift identification. Nine of these redshift identifications also rely on observations from the Atacama Compact Array. The spectroscopic redshifts span a range 1.41 < z < 4.53 with a mean value of 2.75, and the CO emission line full-width at half-maxima range between 110kms−1
Published: 2022

29. GOODS-ALMA 2.0: Source catalog, number counts, and prevailing compact sizes in 1.1 mm galaxies

Author: Gómez-Guijarro, C., Elbaz, D., Xiao, M., Béthermin, M., Franco, M., Magnelli, B., Daddi, E., Dickinson, M., Demarco, R., Inami, H., Rujopakarn, W., Magdis, G.E., Shu, X., Chary, R., Zhou, L., Alexander, D.M., Bournaud, F., Ciesla, L., Ferguson, H.C., Finkelstein, S.L., Finlez, C., Giavalisco, M., Iono, D., Juneau, S., Kartaltepe, J.S., Lagache, G., Le Floc'H, E., Leiton, R., Lin, L., Messias, H., Motohara, K., Mullaney, J., Nagar, N.M., Okumura, K., Pannella, M., Papovich, C., Pope, A., Sargent, M.T., Silverman, J.D., Treister, E., Wang, T., Le Floc’h, E., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Marseille (LAM), 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Hertfordshire [Hatfield] (UH), NSF’s National Optical-Infrared Astronomy Research Laboratory (NOIRLab), Universidad de Concepción - University of Concepcion [Chile], Hiroshima University, Chulalongkorn University [Bangkok], Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Anhui Normal University, California Institute of Technology (CALTECH), Nanjing University (NJU), Durham University, Space Telescope Science Institute (STSci), University of Texas at Austin [Austin], University of Massachusetts [Amherst] (UMass Amherst), University of Massachusetts System (UMASS), National Astronomical Observatory of Japan (NAOJ), Rochester Institute of Technology, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Academia Sinica, The University of Tokyo (UTokyo), University of Sheffield [Sheffield], Università degli studi di Trieste = University of Trieste, Texas A&M University System, University of Sussex, Pontificia Universidad Católica de Chile (UC), Univ New South Wales, MERLin Sch Chem Engn, Sydney, NSW 2052, Australia, and We thank G. Pöpping, C. del P. Lagos, and J. A.Zavala for providing the predicted number counts from their models plotted in Fig. 11. M.F. acknowledges the support from STFC (grant number ST/R000905/1). G.E.M. acknowledges the Villum Fonden research grant 13160 ‘Gas to stars, stars to dust: tracing star formation across cosmic time’ and the Cosmic Dawn Center of Excellence funded by the Danish National Research Foundation under the grant No. 140. H.I. acknowledges support from JSPS KAKENHI Grant Number JP19K23462 and JP21H01129. M.T.S. acknowledges support from a Scientific Exchanges visitor fellowship (IZSEZO_202357) from the Swiss National Science Foundation. This papermakes use of the following ALMA data: ADS/JAO.ALMA#2015.1.00543.S and ADS/JAO.ALMA#2017.1.00755.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We are grateful to the anonymous referee, whose comments have been very useful to improving our work
Subjects: submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, structure [Galaxies], PHYSICAL-PROPERTIES, FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, star formation [Galaxies], 01 natural sciences, GMASS ULTRADEEP SPECTROSCOPY, high-redshift [Galaxies], galaxies [Submillimeter], galaxies: high-redshift, 0103 physical sciences, STAR-FORMING GALAXIES, Sensitivity (control systems), Continuum (set theory), DEEP FIELD-SOUTH, MAIN-SEQUENCE, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Effective radius, Physics, DEGREE EXTRAGALACTIC SURVEY, SUBMILLIMETER GALAXIES, 010308 nuclear & particles physics, photometry [Galaxies], Homogeneity (statistics), MASSIVE GALAXIES, Astronomy and Astrophysics, evolution [Galaxies], FAR-INFRARED PROPERTIES, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: photometry, LUMINOSITY FUNCTION, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, galaxies: structure, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Submillimeter/millimeter observations of dusty star-forming galaxies with the Atacama Large Millimeter/submillimeter Array (ALMA) have shown that dust continuum emission generally occurs in compact regions smaller than the stellar distribution. However, it remains to be understood how systematic these findings are. Studies often lack homogeneity in the sample selection, target discontinuous areas with inhomogeneous sensitivities, and suffer from modest $uv$ coverage coming from single array configurations. GOODS-ALMA is a 1.1mm galaxy survey over a continuous area of 72.42arcmin$^2$ at a homogeneous sensitivity. In this version 2.0, we present a new low resolution dataset and its combination with the previous high resolution dataset from the survey, improving the $uv$ coverage and sensitivity reaching an average of $��= 68.4��$Jy beam$^{-1}$. A total of 88 galaxies are detected in a blind search (compared to 35 in the high resolution dataset alone), 50% at $S/N_{peak} \geq 5$ and 50% at $3.5 \leq S/N_{peak} \leq 5$ aided by priors. Among them, 13 out of the 88 are optically dark or faint sources ($H$- or $K$-band dropouts). The sample dust continuum sizes at 1.1mm are generally compact, with a median effective radius of $R_{e} = 0"10 \pm 0"05$ (a physical size of $R_{e} = 0.73 \pm 0.29$kpc at the redshift of each source). Dust continuum sizes evolve with redshift and stellar mass resembling the trends of the stellar sizes measured at optical wavelengths, albeit a lower normalization compared to those of late-type galaxies. We conclude that for sources with flux densities $S_{1.1mm} > 1$mJy, compact dust continuum emission at 1.1mm prevails, and sizes as extended as typical star-forming stellar disks are rare. The $S_{1.1mm} < 1$mJy sources appear slightly more extended at 1.1mm, although they are still generally compact below the sizes of typical star-forming stellar disks., Accepted by A&A. 30 pages, 18 figures
Published: 2022
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30. The bright extragalactic ALMA redshift survey (BEARS) I: Redshifts of bright gravitationally lensed galaxies from the Herschel ATLAS

Author: Urquhart, SA, Bendo, GJ, Serjeant, S, Bakx, T, Hagimoto, M, Cox, P, Neri, R, Lehnert, M, Sedgwick, C, Weiner, C, Dannerbauer, H, Amvrosiadis, A, Andreani, P, Baker, AJ, Beelen, A, Berta, S, Borsato, E, Buat, V, Butler, KM, Cooray, A, De Zotti, G, Dunne, L, Dye, S, Eales, S, Enia, A, Fan, L, Gavazzi, R, González-Nuevo, J, Harris, AI, Herrera, CN, Hughes, D, Ismail, D, Ivison, R, Jin, S, Jones, B, Kohno, K, Krips, M, Lagache, G, Marchetti, L, Massardi, M, Messias, H, Negrello, M, Omont, A, Perez-Fournon, I, Riechers, DA, Scott, D, Smith, MWL, Stanley, F, Tamura, Y, Temi, P, Vlahakis, C, Weiß, A, Van Der Werf, P, Verma, A, Yang, C, Young, AJ, Urquhart, SA, Bendo, GJ, Serjeant, S, Bakx, T, Hagimoto, M, Cox, P, Neri, R, Lehnert, M, Sedgwick, C, Weiner, C, Dannerbauer, H, Amvrosiadis, A, Andreani, P, Baker, AJ, Beelen, A, Berta, S, Borsato, E, Buat, V, Butler, KM, Cooray, A, De Zotti, G, Dunne, L, Dye, S, Eales, S, Enia, A, Fan, L, Gavazzi, R, González-Nuevo, J, Harris, AI, Herrera, CN, Hughes, D, Ismail, D, Ivison, R, Jin, S, Jones, B, Kohno, K, Krips, M, Lagache, G, Marchetti, L, Massardi, M, Messias, H, Negrello, M, Omont, A, Perez-Fournon, I, Riechers, DA, Scott, D, Smith, MWL, Stanley, F, Tamura, Y, Temi, P, Vlahakis, C, Weiß, A, Van Der Werf, P, Verma, A, Yang, C, and Young, AJ
Abstract: We present spectroscopic measurements for 71 galaxies associated with 62 of the brightest high-redshift submillimetre sources from the Southern fields of the Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS), while targeting 85 sources which resolved into 142. We have obtained robust redshift measurements for all sources using the 12-m Array and an efficient tuning of ALMA to optimize its use as a redshift hunter, with 73 per cent of the sources having a robust redshift identification. Nine of these redshift identifications also rely on observations from the Atacama Compact Array. The spectroscopic redshifts span a range 1.41 < z < 4.53 with a mean value of 2.75, and the CO emission line full-width at half-maxima range between $\rm 110\, km\, s^{-1} \lt FWHM \lt 1290\, km\, s^{-1}$ with a mean value of ∼500 km s−1, in line with other high-z samples. The derived CO(1-0) luminosity is significantly elevated relative to line-width to CO(1-0) luminosity scaling relation, which is suggestive of lensing magnification across our sources. In fact, the distribution of magnification factors inferred from the CO equivalent widths is consistent with expectations from galaxy–galaxy lensing models, though there is a hint of an excess at large magnifications that may be attributable to the additional lensing optical depth from galaxy groups or clusters.
Published: 2022

31. Orbital motion near Sagittarius A*: Constraints from polarimetric ALMA observations

Author: Wielgus, M., Moscibrodzka, M.A., Vos, J., Gelles, Z., Marti-Vidal, I, Farah, J., Goddi, C., Messias, H., Wielgus, M., Moscibrodzka, M.A., Vos, J., Gelles, Z., Marti-Vidal, I, Farah, J., Goddi, C., and Messias, H.
Abstract: Contains fulltext : 281840.pdf (Publisher’s version ) (Open Access)
Published: 2022

32. The bright extragalactic ALMA redshift survey (BEARS) I: redshifts of bright gravitationally lensed galaxies from the Herschel ATLAS

Author: Urquhart, S A, primary, Bendo, G J, additional, Serjeant, S, additional, Bakx, T, additional, Hagimoto, M, additional, Cox, P, additional, Neri, R, additional, Lehnert, M, additional, Sedgwick, C, additional, Weiner, C, additional, Dannerbauer, H, additional, Amvrosiadis, A, additional, Andreani, P, additional, Baker, A J, additional, Beelen, A, additional, Berta, S, additional, Borsato, E, additional, Buat, V, additional, Butler, K M, additional, Cooray, A, additional, De Zotti, G, additional, Dunne, L, additional, Dye, S, additional, Eales, S, additional, Enia, A, additional, Fan, L, additional, Gavazzi, R, additional, González-Nuevo, J, additional, Harris, A I, additional, Herrera, C N, additional, Hughes, D, additional, Ismail, D, additional, Ivison, R, additional, Jin, S, additional, Jones, B, additional, Kohno, K, additional, Krips, M, additional, Lagache, G, additional, Marchetti, L, additional, Massardi, M, additional, Messias, H, additional, Negrello, M, additional, Omont, A, additional, Perez-Fournon, I, additional, Riechers, D A, additional, Scott, D, additional, Smith, M W L, additional, Stanley, F, additional, Tamura, Y, additional, Temi, P, additional, Vlahakis, C, additional, Weiß, A, additional, van der Werf, P, additional, Verma, A, additional, Yang, C, additional, and Young, A J, additional
Published: 2022
Full Text: View/download PDF

33. Epidemiological, clinical and laboratory aspects of Angiostrongylus cantonensis infection: an integrative review

Author: Carvalho, M. S. N., primary, Carvalho, M. R., additional, Santos, J. A. O., additional, Barbosa, N. D., additional, Melo, L. C., additional, Costa, F. H. M., additional, Carvalho, J. P. F., additional, Messias, H. B. G., additional, Fonseca, S. A., additional, Souza, M. A., additional, Ferreira-Júnior, G. C., additional, Lima, R. F., additional, Costa, J. G., additional, Cavalcanti, M. G. S., additional, and Matos-Rocha, T. J., additional
Published: 2022
Full Text: View/download PDF

34. First Sagittarius A* Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole in the Center of the Milky Way

Author: null Event Horizon Telescope Collaboration, Kazunori Akiyama, Antxon Alberdi, Walter Alef, Juan Carlos Algaba, Richard Anantua, Keiichi Asada, Rebecca Azulay, Uwe Bach, Anne-Kathrin Baczko, David Ball, Mislav Baloković, John Barrett, Michi Bauböck, Bradford A. Benson, Dan Bintley, Lindy Blackburn, Raymond Blundell, Katherine L. Bouman, Geoffrey C. Bower, Hope Boyce, Michael Bremer, Christiaan D. Brinkerink, Roger Brissenden, Silke Britzen, Avery E. Broderick, Dominique Broguiere, Thomas Bronzwaer, Sandra Bustamante, Do-Young Byun, John E. Carlstrom, Chiara Ceccobello, Andrew Chael, Chi-kwan Chan, Koushik Chatterjee, Shami Chatterjee, Ming-Tang Chen, Yongjun Chen, Xiaopeng Cheng, Ilje Cho, Pierre Christian, Nicholas S. Conroy, John E. Conway, James M. Cordes, Thomas M. Crawford, Geoffrey B. Crew, Alejandro Cruz-Osorio, Yuzhu Cui, Jordy Davelaar, Mariafelicia De Laurentis, Roger Deane, Jessica Dempsey, Gregory Desvignes, Jason Dexter, Vedant Dhruv, Sheperd S. Doeleman, Sean Dougal, Sergio A. Dzib, Ralph P. Eatough, Razieh Emami, Heino Falcke, Joseph Farah, Vincent L. Fish, Ed Fomalont, H. Alyson Ford, Raquel Fraga-Encinas, William T. Freeman, Per Friberg, Christian M. Fromm, Antonio Fuentes, Peter Galison, Charles F. Gammie, Roberto García, Olivier Gentaz, Boris Georgiev, Ciriaco Goddi, Roman Gold, Arturo I. Gómez-Ruiz, José L. Gómez, Minfeng Gu, Mark Gurwell, Kazuhiro Hada, Daryl Haggard, Kari Haworth, Michael H. Hecht, Ronald Hesper, Dirk Heumann, Luis C. Ho, Paul Ho, Mareki Honma, Chih-Wei L. Huang, Lei Huang, David H. Hughes, Shiro Ikeda, C. M. Violette Impellizzeri, Makoto Inoue, Sara Issaoun, David J. James, Buell T. Jannuzi, Michael Janssen, Britton Jeter, Wu Jiang, Alejandra Jiménez-Rosales, Michael D. Johnson, Svetlana Jorstad, Abhishek V. Joshi, Taehyun Jung, Mansour Karami, Ramesh Karuppusamy, Tomohisa Kawashima, Garrett K. Keating, Mark Kettenis, Dong-Jin Kim, Jae-Young Kim, Jongsoo Kim, Junhan Kim, Motoki Kino, Jun Yi Koay, Prashant Kocherlakota, Yutaro Kofuji, Patrick M. Koch, Shoko Koyama, Carsten Kramer, Michael Kramer, Thomas P. Krichbaum, Cheng-Yu Kuo, Noemi La Bella, Tod R. Lauer, Daeyoung Lee, Sang-Sung Lee, Po Kin Leung, Aviad Levis, Zhiyuan Li, Rocco Lico, Greg Lindahl, Michael Lindqvist, Mikhail Lisakov, Jun Liu, Kuo Liu, Elisabetta Liuzzo, Wen-Ping Lo, Andrei P. Lobanov, Laurent Loinard, Colin J. Lonsdale, Ru-Sen Lu, Jirong Mao, Nicola Marchili, Sera Markoff, Daniel P. Marrone, Alan P. Marscher, Iván Martí-Vidal, Satoki Matsushita, Lynn D. Matthews, Lia Medeiros, Karl M. Menten, Daniel Michalik, Izumi Mizuno, Yosuke Mizuno, James M. Moran, Kotaro Moriyama, Monika Moscibrodzka, Cornelia Müller, Alejandro Mus, Gibwa Musoke, Ioannis Myserlis, Andrew Nadolski, Hiroshi Nagai, Neil M. Nagar, Masanori Nakamura, Ramesh Narayan, Gopal Narayanan, Iniyan Natarajan, Antonios Nathanail, Santiago Navarro Fuentes, Joey Neilsen, Roberto Neri, Chunchong Ni, Aristeidis Noutsos, Michael A. Nowak, Junghwan Oh, Hiroki Okino, Héctor Olivares, Gisela N. Ortiz-León, Tomoaki Oyama, Feryal Özel, Daniel C. M. Palumbo, Georgios Filippos Paraschos, Jongho Park, Harriet Parsons, Nimesh Patel, Ue-Li Pen, Dominic W. Pesce, Vincent Piétu, Richard Plambeck, Aleksandar PopStefanija, Oliver Porth, Felix M. Pötzl, Ben Prather, Jorge A. Preciado-López, Dimitrios Psaltis, Hung-Yi Pu, Venkatessh Ramakrishnan, Ramprasad Rao, Mark G. Rawlings, Alexander W. Raymond, Luciano Rezzolla, Angelo Ricarte, Bart Ripperda, Freek Roelofs, Alan Rogers, Eduardo Ros, Cristina Romero-Cañizales, Arash Roshanineshat, Helge Rottmann, Alan L. Roy, Ignacio Ruiz, Chet Ruszczyk, Kazi L. J. Rygl, Salvador Sánchez, David Sánchez-Argüelles, Miguel Sánchez-Portal, Mahito Sasada, Kaushik Satapathy, Tuomas Savolainen, F. Peter Schloerb, Jonathan Schonfeld, Karl-Friedrich Schuster, Lijing Shao, Zhiqiang Shen, Des Small, Bong Won Sohn, Jason SooHoo, Kamal Souccar, He Sun, Fumie Tazaki, Alexandra J. Tetarenko, Paul Tiede, Remo P. J. Tilanus, Michael Titus, Pablo Torne, Efthalia Traianou, Tyler Trent, Sascha Trippe, Matthew Turk, Ilse van Bemmel, Huib Jan van Langevelde, Daniel R. van Rossum, Jesse Vos, Jan Wagner, Derek Ward-Thompson, John Wardle, Jonathan Weintroub, Norbert Wex, Robert Wharton, Maciek Wielgus, Kaj Wiik, Gunther Witzel, Michael F. Wondrak, George N. Wong, Qingwen Wu, Paul Yamaguchi, Doosoo Yoon, André Young, Ken Young, Ziri Younsi, Feng Yuan, Ye-Fei Yuan, J. Anton Zensus, Shuo Zhang, Guang-Yao Zhao, Shan-Shan Zhao, Claudio Agurto, Alexander Allardi, Rodrigo Amestica, Juan Pablo Araneda, Oriel Arriagada, Jennie L. Berghuis, Alessandra Bertarini, Ryan Berthold, Jay Blanchard, Ken Brown, Mauricio Cárdenas, Michael Cantzler, Patricio Caro, Edgar Castillo-Domínguez, Tin Lok Chan, Chih-Cheng Chang, Dominic O. Chang, Shu-Hao Chang, Song-Chu Chang, Chung-Chen Chen, Ryan Chilson, Tim C. Chuter, Miroslaw Ciechanowicz, Edgar Colin-Beltran, Iain M. Coulson, Joseph Crowley, Nathalie Degenaar, Sven Dornbusch, Carlos A. Durán, Wendeline B. Everett, Aaron Faber, Karl Forster, Miriam M. Fuchs, David M. Gale, Gertie Geertsema, Edouard González, Dave Graham, Frédéric Gueth, Nils W. Halverson, Chih-Chiang Han, Kuo-Chang Han, Yutaka Hasegawa, José Luis Hernández-Rebollar, Cristian Herrera, Ruben Herrero-Illana, Stefan Heyminck, Akihiko Hirota, James Hoge, Shelbi R. Hostler Schimpf, Ryan E. Howie, Yau-De Huang, Homin Jiang, Hao Jinchi, David John, Kimihiro Kimura, Thomas Klein, Derek Kubo, John Kuroda, Caleb Kwon, Richard Lacasse, Robert Laing, Erik M. Leitch, Chao-Te Li, Ching-Tang Liu, Kuan-Yu Liu, Lupin C.-C. Lin, Li-Ming Lu, Felipe Mac-Auliffe, Pierre Martin-Cocher, Callie Matulonis, John K. Maute, Hugo Messias, Zheng Meyer-Zhao, Alfredo Montaña, Francisco Montenegro-Montes, William Montgomerie, Marcos Emir Moreno Nolasco, Dirk Muders, Hiroaki Nishioka, Timothy J. Norton, George Nystrom, Hideo Ogawa, Rodrigo Olivares, Peter Oshiro, Juan Pablo Pérez-Beaupuits, Rodrigo Parra, Neil M. Phillips, Michael Poirier, Nicolas Pradel, Richard Qiu, Philippe A. Raffin, Alexandra S. Rahlin, Jorge Ramírez, Sean Ressler, Mark Reynolds, Iván Rodríguez-Montoya, Alejandro F. Saez-Madain, Jorge Santana, Paul Shaw, Leslie E. Shirkey, Kevin M. Silva, William Snow, Don Sousa, T. K. Sridharan, William Stahm, Anthony A. Stark, John Test, Karl Torstensson, Paulina Venegas, Craig Walther, Ta-Shun Wei, Chris White, Gundolf Wieching, Rudy Wijnands, Jan G. A. Wouterloot, Chen-Yu Yu, Wei Yu (于威), Milagros Zeballos, High Energy Astrophys. & Astropart. Phys (API, FNWI), Akiyama, K., Alberdi, A., Alef, W., Algaba, J. C., Anantua, R., Azulay, R., Asada, K., Bach, U., Baczko, A. -K., Ball, D., Balokovic, M., Barrett, J., Baubock, M., Benson, B. A., Bintley, D., Blackburn, L., Blundell, R., Bouman, K. L., Bower, G. C., Boyce, H., Bremer, M., Brinkerink, C. D., Brissenden, R., Britzen, S., Broderick, A. E., Broguiere, D., Bronzwaer, T., Bustamante, S., Byun, D. -Y., Carlstrom, J. E., Ceccobello, C., Chael, A., Chan, C. -K., Chatterjee, K., Chatterjee, S., Chen, M. -T., Chen, Y., Cheng, X., Cho, I., Christian, P., Conroy, N. S., Conway, J. E., Cordes, J. M., Crawford, T. M., Crew, G. B., Cruz-Osorio, A., Cui, Y., Davelaar, J., De Laurentis, M., Deane, R., Dempsey, J., Desvignes, G., Dexter, J., Dhruv, V., Doeleman, S. S., Dougal, S., Dzib, S. A., Eatough, R. P., Emami, R., Falcke, H., Farah, J., Fish, V. L., Fomalont, E., Ford, H. A., Fraga-Encinas, R., Freeman, W. T., Friberg, P., Fromm, C. M., Fuentes, A., Galison, P., Gammie, C. F., Gentaz, O., Georgiev, B., Garcia, R., Goddi, C., Gold, R., Gomez-Ruiz, A. I., Gomez, J. L., Gu, M., Gurwell, M., Hada, K., Haggard, D., Haworth, K., Hecht, M. H., Hesper, R., Heumann, D., Ho, L. C., Ho, P., Honma, M., Huang, C. -W. L., Huang, L., Hughes, D. H., Ikeda, S., Impellizzeri, C. M. V., Inoue, M., Issaoun, S., James, D. J., Jannuzi, B. T., Janssen, M., Jeter, B., Jiang, W., Jimenez-Rosales, A., Johnson, M. D., Jorstad, S., Joshi, A. V., Jung, T., Karami, M., Karuppusamy, R., Kawashima, T., Keating, G. K., Kettenis, M., Kim, D. -J., Kim, J. -Y., Kim, J., Kino, M., Koay, J. Y., Kocherlakota, P., Kofuji, Y., Koch, P. M., Koyama, S., Kramer, C., Kramer, M., Krichbaum, T. P., Kuo, C. -Y., La Bella, N., Lauer, T. R., Lee, D., Lee, S. -S., Leung, P. K., Levis, A., Li, Z., Lico, R., Lindahl, G., Lindqvist, M., Lisakov, M., Liu, J., Liu, K., Liuzzo, E., Lo, W. -P., Lobanov, A. P., Loinard, L., Lonsdale, C. J., Lu, R. -S., Mao, J., Marchili, N., Markoff, S., Marrone, D. P., Marscher, A. P., Marti-Vidal, I., Matsushita, S., Matthews, L. D., Medeiros, L., Menten, K. M., Michalik, D., Mizuno, I., Mizuno, Y., Moran, J. M., Moriyama, K., Moscibrodzka, M., Muller, C., Mus, A., Musoke, G., Myserlis, I., Nadolski, A., Nagai, H., Nagar, N. M., Nakamura, M., Narayan, R., Narayanan, G., Natarajan, I., Nathanail, A., Fuentes, S. N., Neilsen, J., Neri, R., Ni, C., Noutsos, A., Nowak, M. A., Oh, J., Okino, H., Olivares, H., Ortiz-Leon, G. N., Oyama, T., Ozel, F., Palumbo, D. C. M., Paraschos, G. F., Park, J., Parsons, H., Patel, N., Pen, U. -L., Pesce, D. W., Pietu, V., Plambeck, R., Popstefanija, A., Porth, O., Potzl, F. M., Prather, B., Preciado-Lopez, J. A., Psaltis, D., Pu, H. -Y., Ramakrishnan, V., Rao, R., Rawlings, M. G., Raymond, A. W., Rezzolla, L., Ricarte, A., Ripperda, B., Roelofs, F., Rogers, A., Ros, E., Romero-Canizales, C., Roshanineshat, A., Rottmann, H., Roy, A. L., Ruiz, I., Ruszczyk, C., Rygl, K. L. J., Sanchez, S., Sanchez-Arguelles, D., Sanchez-Portal, M., Sasada, M., Satapathy, K., Savolainen, T., Schloerb, F. P., Schonfeld, J., Schuster, K. -F., Shao, L., Shen, Z., Small, D., Sohn, B. W., Soohoo, J., Souccar, K., Sun, H., Tazaki, F., Tetarenko, A. J., Tilanus, R. P. J., Tiede, P., Titus, M., Torne, P., Traianou, E., Trent, T., Trippe, S., Turk, M., van Bemmel, I., van Langevelde, H. J., van Rossum, D. R., Vos, J., Wagner, J., Ward-Thompson, D., Wardle, J., Weintroub, J., Wex, N., Wharton, R., Wielgus, M., Wiik, K., Witzel, G., Wondrak, M. F., Wong, G. N., Wu, Q., Yamaguchi, P., Yoon, D., Young, A., Young, K., Younsi, Z., Yuan, F., Yuan, Y. -F., Zensus, J. A., Zhang, S., Zhao, G. -Y., Zhao, S. -S., Agurto, C., Allardi, A., Amestica, R., Araneda, J. P., Arriagada, O., Berghuis, J. L., Bertarini, A., Berthold, R., Blanchard, J., Brown, K., Cardenas, M., Cantzler, M., Caro, P., Castillo-Dominguez, E., Chan, T. L., Chang, C. -C., Chang, D. O., Chang, S. -H., Chang, S. -C., Chen, C. -C., Chilson, R., Chuter, T. C., Ciechanowicz, M., Colin-Beltran, E., Coulson, I. M., Crowley, J., Degenaar, N., Dornbusch, S., Duran, C. A., Everett, W. B., Faber, A., Forster, K., Fuchs, M. M., Gale, D. M., Geertsema, G., Gonzalez, E., Graham, D., Gueth, F., Halverson, N. W., Han, C. -C., Han, K. -C., Hasegawa, Y., Hernandez-Rebollar, J. L., Herrera, C., Herrero-Illana, R., Heyminck, S., Hirota, A., Hoge, J., Hostler Schimpf, S. R., Howie, R. E., Huang, Y. -D., Jiang, H., Jinchi, H., John, D., Kimura, K., Klein, T., Kubo, D., Kuroda, J., Kwon, C., Lacasse, R., Laing, R., Leitch, E. M., Li, C. -T., Liu, C. -T., Liu, K. -Y., Lin, L. C. -C., Lu, L. -M., Mac-Auliffe, F., Martin-Cocher, P., Matulonis, C., Maute, J. K., Messias, H., Meyer-Zhao, Z., Montana, A., Montenegro-Montes, F., Montgomerie, W., Nolasco, M. E. M., Muders, D., Nishioka, H., Norton, T. J., Nystrom, G., Ogawa, H., Olivares, R., Oshiro, P., Perez-Beaupuits, J. P., Parra, R., Phillips, N. M., Poirier, M., Pradel, N., Qiu, R., Raffin, P. A., Rahlin, A. S., Ramirez, J., Ressler, S., Reynolds, M., Rodriguez-Montoya, I., Saez-Madain, A. F., Santana, J., Shaw, P., Shirkey, L. E., Silva, K. M., Snow, W., Sousa, D., Sridharan, T. K., Stahm, W., Stark, A. A., Test, J., Torstensson, K., Venegas, P., Walther, C., Wei, T. -S., White, C., Wieching, G., Wijnands, R., Wouterloot, J. G. A., Yu, C. -Y., Yu, W., Zeballos, M., Akiyama, Kazunori [0000-0002-9475-4254], Alberdi, Antxon [0000-0002-9371-1033], Algaba, Juan Carlos [0000-0001-6993-1696], Anantua, Richard [0000-0003-3457-7660], Asada, Keiichi [0000-0001-6988-8763], Azulay, Rebecca [0000-0002-2200-5393], Bach, Uwe [0000-0002-7722-8412], Baczko, Anne-Kathrin [0000-0003-3090-3975], Baloković, Mislav [0000-0003-0476-6647], Barrett, John [0000-0002-9290-0764], Bauböck, Michi [0000-0002-5518-2812], Benson, Bradford A. [0000-0002-5108-6823], Blackburn, Lindy [0000-0002-9030-642X], Blundell, Raymond [0000-0002-5929-5857], Bouman, Katherine L. [0000-0003-0077-4367], Bower, Geoffrey C. [0000-0003-4056-9982], Boyce, Hope [0000-0002-6530-5783], Brinkerink, Christiaan D. [0000-0002-2322-0749], Brissenden, Roger [0000-0002-2556-0894], Britzen, Silke [0000-0001-9240-6734], Broderick, Avery E. [0000-0002-3351-760X], Broguiere, Dominique [0000-0001-9151-6683], Bronzwaer, Thomas [0000-0003-1151-3971], Bustamante, Sandra [0000-0001-6169-1894], Byun, Do-Young [0000-0003-1157-4109], Carlstrom, John E. [0000-0002-2044-7665], Ceccobello, Chiara [0000-0002-4767-9925], Chael, Andrew [0000-0003-2966-6220], Chan, Chi-kwan [0000-0001-6337-6126], Chatterjee, Koushik [0000-0002-2825-3590], Chatterjee, Shami [0000-0002-2878-1502], Chen, Ming-Tang [0000-0001-6573-3318], Chen, Yongjun [0000-0001-5650-6770], Cheng, Xiaopeng [0000-0003-4407-9868], Cho, Ilje [0000-0001-6083-7521], Christian, Pierre [0000-0001-6820-9941], Conroy, Nicholas S. [0000-0003-2886-2377], Conway, John E. [0000-0003-2448-9181], Cordes, James M. [0000-0002-4049-1882], Crawford, Thomas M. [0000-0001-9000-5013], Crew, Geoffrey B. [0000-0002-2079-3189], Cruz-Osorio, Alejandro [0000-0002-3945-6342], Cui, Yuzhu [0000-0001-6311-4345], Davelaar, Jordy [0000-0002-2685-2434], Laurentis, Mariafelicia De [0000-0002-9945-682X], Deane, Roger [0000-0003-1027-5043], Dempsey, Jessica [0000-0003-1269-9667], Desvignes, Gregory [0000-0003-3922-4055], Dexter, Jason [0000-0003-3903-0373], Dhruv, Vedant [0000-0001-6765-877X], Doeleman, Sheperd S. [0000-0002-9031-0904], Dougal, Sean [0000-0002-3769-1314], Dzib, Sergio A. [0000-0001-6010-6200], Eatough, Ralph P. [0000-0001-6196-4135], Emami, Razieh [0000-0002-2791-5011], Falcke, Heino [0000-0002-2526-6724], Farah, Joseph [0000-0003-4914-5625], Fish, Vincent L. [0000-0002-7128-9345], Fomalont, Ed [0000-0002-9036-2747], Ford, H. Alyson [0000-0002-9797-0972], Fraga-Encinas, Raquel [0000-0002-5222-1361], Friberg, Per [0000-0002-8010-8454], Fromm, Christian M. [0000-0002-1827-1656], Fuentes, Antonio [0000-0002-8773-4933], Galison, Peter [0000-0002-6429-3872], Gammie, Charles F. [0000-0001-7451-8935], García, Roberto [0000-0002-6584-7443], Gentaz, Olivier [0000-0002-0115-4605], Georgiev, Boris [0000-0002-3586-6424], Goddi, Ciriaco [0000-0002-2542-7743], Gold, Roman [0000-0003-2492-1966], Gómez-Ruiz, Arturo I. [0000-0001-9395-1670], Gómez, José L. [0000-0003-4190-7613], Gu, Minfeng [0000-0002-4455-6946], Gurwell, Mark [0000-0003-0685-3621], Hada, Kazuhiro [0000-0001-6906-772X], Haggard, Daryl [0000-0001-6803-2138], Hecht, Michael H. [0000-0002-4114-4583], Hesper, Ronald [0000-0003-1918-6098], Heumann, Dirk [0000-0002-7671-0047], Ho, Luis C. [0000-0001-6947-5846], Ho, Paul [0000-0002-3412-4306], Honma, Mareki [0000-0003-4058-9000], Huang, Chih-Wei L. [0000-0001-5641-3953], Huang, Lei [0000-0002-1923-227X], Ikeda, Shiro [0000-0002-2462-1448], Impellizzeri, C. M. Violette [0000-0002-3443-2472], Inoue, Makoto [0000-0001-5037-3989], Issaoun, Sara [0000-0002-5297-921X], James, David J. [0000-0001-5160-4486], Jannuzi, Buell T. [0000-0002-1578-6582], Janssen, Michael [0000-0001-8685-6544], Jeter, Britton [0000-0003-2847-1712], Jiang, Wu [0000-0001-7369-3539], Jiménez-Rosales, Alejandra [0000-0002-2662-3754], Johnson, Michael D. [0000-0002-4120-3029], Jorstad, Svetlana [0000-0001-6158-1708], Joshi, Abhishek V. [0000-0002-2514-5965], Jung, Taehyun [0000-0001-7003-8643], Karami, Mansour [0000-0001-7387-9333], Karuppusamy, Ramesh [0000-0002-5307-2919], Kawashima, Tomohisa [0000-0001-8527-0496], Keating, Garrett K. [0000-0002-3490-146X], Kettenis, Mark [0000-0002-6156-5617], Kim, Dong-Jin [0000-0002-7038-2118], Kim, Jae-Young [0000-0001-8229-7183], Kim, Jongsoo [0000-0002-1229-0426], Kim, Junhan [0000-0002-4274-9373], Kino, Motoki [0000-0002-2709-7338], Koay, Jun Yi [0000-0002-7029-6658], Kocherlakota, Prashant [0000-0001-7386-7439], Koch, Patrick M. [0000-0003-2777-5861], Koyama, Shoko [0000-0002-3723-3372], Kramer, Carsten [0000-0002-4908-4925], Kramer, Michael [0000-0002-4175-2271], Krichbaum, Thomas P. [0000-0002-4892-9586], Kuo, Cheng-Yu [0000-0001-6211-5581], Bella, Noemi La [0000-0002-8116-9427], Lauer, Tod R. [0000-0003-3234-7247], Lee, Daeyoung [0000-0002-3350-5588], Lee, Sang-Sung [0000-0002-6269-594X], Leung, Po Kin [0000-0002-8802-8256], Levis, Aviad [0000-0001-7307-632X], Li, Zhiyuan [0000-0003-0355-6437], Lico, Rocco [0000-0001-7361-2460], Lindahl, Greg [0000-0002-6100-4772], Lindqvist, Michael [0000-0002-3669-0715], Lisakov, Mikhail [0000-0001-6088-3819], Liu, Jun [0000-0002-7615-7499], Liu, Kuo [0000-0002-2953-7376], Liuzzo, Elisabetta [0000-0003-0995-5201], Lo, Wen-Ping [0000-0003-1869-2503], Lobanov, Andrei P. [0000-0003-1622-1484], Loinard, Laurent [0000-0002-5635-3345], Lonsdale, Colin J. [0000-0003-4062-4654], Lu, Ru-Sen [0000-0002-7692-7967], Mao, Jirong [0000-0002-7077-7195], Marchili, Nicola [0000-0002-5523-7588], Markoff, Sera [0000-0001-9564-0876], Marrone, Daniel P. [0000-0002-2367-1080], Marscher, Alan P. [0000-0001-7396-3332], Martí-Vidal, Iván [0000-0003-3708-9611], Matsushita, Satoki [0000-0002-2127-7880], Matthews, Lynn D. [0000-0002-3728-8082], Medeiros, Lia [0000-0003-2342-6728], Menten, Karl M. [0000-0001-6459-0669], Michalik, Daniel [0000-0002-7618-6556], Mizuno, Izumi [0000-0002-7210-6264], Mizuno, Yosuke [0000-0002-8131-6730], Moran, James M. [0000-0002-3882-4414], Moriyama, Kotaro [0000-0003-1364-3761], Moscibrodzka, Monika [0000-0002-4661-6332], Müller, Cornelia [0000-0002-2739-2994], Mus, Alejandro [0000-0003-0329-6874], Musoke, Gibwa [0000-0003-1984-189X], Myserlis, Ioannis [0000-0003-3025-9497], Nadolski, Andrew [0000-0001-9479-9957], Nagai, Hiroshi [0000-0003-0292-3645], Nagar, Neil M. 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[0000-0001-6952-2147], Wu, Qingwen [0000-0003-4773-4987], Yamaguchi, Paul [0000-0002-6017-8199], Yoon, Doosoo [0000-0001-8694-8166], Young, André [0000-0003-0000-2682], Young, Ken [0000-0002-3666-4920], Younsi, Ziri [0000-0001-9283-1191], Yuan, Feng [0000-0003-3564-6437], Yuan, Ye-Fei [0000-0002-7330-4756], Zensus, J. Anton [0000-0001-7470-3321], Zhang, Shuo [0000-0002-2967-790X], Zhao, Guang-Yao [0000-0002-4417-1659], Zhao, Shan-Shan [0000-0002-9774-3606], Berghuis, Jennie L. [0000-0003-2287-158X], Blanchard, Jay [0000-0002-2756-395X], Chan, Tin Lok [0000-0001-9197-932X], Coulson, Iain M. [0000-0002-7316-4626], Degenaar, Nathalie [0000-0002-0092-3548], Durán, Carlos A. [0000-0001-7622-3890], Everett, Wendeline B. [0000-0002-5370-6651], Forster, Karl [0000-0001-5800-5531], Halverson, Nils W. [0000-0003-2606-9340], Herrero-Illana, Ruben [0000-0002-7758-8717], Hirota, Akihiko [0000-0002-0465-5421], Howie, Ryan E. [0000-0002-5451-3624], Kwon, Caleb [0000-0001-9006-7345], Laing, Robert [0000-0001-6786-3087], Leitch, Erik M. [0000-0001-8553-9336], Lin, Lupin C.-C. [0000-0003-4083-9567], Maute, John K. [0000-0002-5744-4249], Messias, Hugo [0000-0002-2985-7994], Montenegro-Montes, Francisco [0000-0002-7430-3771], Muders, Dirk [0000-0002-2315-2571], Pérez-Beaupuits, Juan Pablo [0000-0003-3536-2274], Poirier, Michael [0000-0001-6641-0959], Qiu, Richard [0000-0003-3462-0817], Rahlin, Alexandra S. [0000-0003-3953-1776], Ressler, Sean [0000-0003-0220-5723], Reynolds, Mark [0000-0003-1621-9392], Saez-Madain, Alejandro F. [0000-0002-0804-3414], Sousa, Don [0000-0002-2625-2607], Stark, Anthony A. [0000-0002-2718-9996], White, Chris [0000-0001-7448-4253], Wijnands, Rudy [0000-0002-3516-2152], Wouterloot, Jan G. A. [0000-0002-4694-6905], Yu (于威), Wei [0000-0002-5168-6052], Apollo - University of Cambridge Repository, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Science and Technology Facilities Council (UK), Astronomy, Metsähovi Radio Observatory, Department of Electronics and Nanoengineering, Science Support Office, Aalto-yliopisto, and Aalto University
Subjects: Black holes, F520, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, F521, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 5109 Space Sciences, Heterodyne interferometry, Galactic center, General Relativity and Quantum Cosmology, Space and Planetary Science, 5101 Astronomical Sciences, Kerr black holes, Rotating black holes, 51 Physical Sciences, Astrophysics::Galaxy Astrophysics, Mathematics
Abstract: This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited. Full list of authors: Akiyama, Kazunori; Alberdi, Antxon; Alef, Walter; Algaba, Juan Carlos; Anantua, Richard; Asada, Keiichi; Azulay, Rebecca; Bach, Uwe; Baczko, Anne-Kathrin; Ball, David; Balokovic, Mislav; Barrett, John; Baubock, Michi; Benson, Bradford A.; Bintley, Dan; Blackburn, Lindy; Blundell, Raymond; Bouman, Katherine L.; Bower, Geoffrey C.; Boyce, Hope; Bremer, Michael; Brinkerink, Christiaan D.; Brissenden, Roger; Britzen, Silke; Broderick, Avery E.; Broguiere, Dominique; Bronzwaer, Thomas; Bustamante, Sandra; Byun, Do-Young; Carlstrom, John E.; Ceccobello, Chiara; Chael, Andrew; Chan, Chi-kwan; Chatterjee, Koushik; Chatterjee, Shami; Chen, Ming-Tang; Chen, Yongjun; Cheng, Xiaopeng; Cho, Ilje; Christian, Pierre; Conroy, Nicholas S.; Conway, John E.; Cordes, James M.; Crawford, Thomas M.; Crew, Geoffrey B.; Cruz-Osorio, Alejandro; Cui, Yuzhu; Davelaar, Jordy; De Laurentis, Mariafelicia; Deane, Roger; Dempsey, Jessica; Desvignes, Gregory; Dexter, Jason; Dhruv, Vedant; Doeleman, Sheperd S.; Dougal, Sean; Dzib, Sergio A.; Eatough, Ralph P.; Emami, Razieh; Falcke, Heino; Farah, Joseph; Fish, Vincent L.; Fomalont, Ed; Ford, H. Alyson; Fraga-Encinas, Raquel; Freeman, William T.; Friberg, Per; Fromm, Christian M.; Fuentes, Antonio; Galison, Peter; Gammie, Charles F.; Garcia, Roberto; Gentaz, Olivier; Georgiev, Boris; Goddi, Ciriaco; Gold, Roman; Gomez-Ruiz, Arturo, I; Gomez, Jose L.; Gu, Minfeng; Gurwell, Mark; Hada, Kazuhiro; Haggard, Daryl; Haworth, Kari; Hecht, Michael H.; Hesper, Ronald; Heumann, Dirk; Ho, Luis C.; Ho, Paul; Honma, Mareki; Huang, Chih-Wei L.; Huang, Lei; Hughes, David H.; Ikeda, Shiro; Impellizzeri, C. M. Violette; Inoue, Makoto; Issaoun, Sara; James, David J.; Jannuzi, Buell T.; Janssen, Michael; Jeter, Britton; Jiang, Wu; Jimenez-Rosales, Alejandra; Johnson, Michael D.; Jorstad, Svetlana; Joshi, Abhishek, V; Jung, Taehyun; Karami, Mansour; Karuppusamy, Ramesh; Kawashima, Tomohisa; Keating, Garrett K.; Kettenis, Mark; Kim, Dong-Jin; Kim, Jae-Young; Kim, Jongsoo; Kim, Junhan; Kino, Motoki; Koay, Jun Yi; Kocherlakota, Prashant; Kofuji, Yutaro; Koch, Patrick M.; Koyama, Shoko; Kramer, Carsten; Kramer, Michael; Krichbaum, Thomas P.; Kuo, Cheng-Yu; La Bella, Noemi; Lauer, Tod R.; Lee, Daeyoung; Lee, Sang-Sung; Leung, Po Kin; Levis, Aviad; Li, Zhiyuan; Lico, Rocco; Lindahl, Greg; Lindqvist, Michael; Lisakov, Mikhail; Liu, Jun; Liu, Kuo; Liuzzo, Elisabetta; Lo, Wen-Ping; Lobanov, Andrei P.; Loinard, Laurent; Lonsdale, Colin J.; Lu, Ru-Sen; Mao, Jirong; Marchili, Nicola; Markoff, Sera; Marrone, Daniel P.; Marscher, Alan P.; Marti-Vidal, Ivan; Matsushita, Satoki; Matthews, Lynn D.; Medeiros, Lia; Menten, Karl M.; Michalik, Daniel; Mizuno, Izumi; Mizuno, Yosuke; Moran, James M.; Moriyama, Kotaro; Moscibrodzka, Monika; Muller, Cornelia; Mus, Alejandro; Musoke, Gibwa; Myserlis, Ioannis; Nadolski, Andrew; Nagai, Hiroshi; Nagar, Neil M.; Nakamura, Masanori; Narayan, Ramesh; Narayanan, Gopal; Natarajan, Iniyan; Nathanail, Antonios; Fuentes, Santiago Navarro; Neilsen, Joey; Neri, Roberto; Ni, Chunchong; Noutsos, Aristeidis; Nowak, Michael A.; Oh, Junghwan; Okino, Hiroki; Olivares, Hector; Ortiz-Leon, Gisela N.; Oyama, Tomoaki; Palumbo, Daniel C. M.; Paraschos, Georgios Filippos; Park, Jongho; Parsons, Harriet; Patel, Nimesh; Pen, Ue-Li; Pesce, Dominic W.; Pietu, Vincent; Plambeck, Richard; PopStefanija, Aleksandar; Porth, Oliver; Potzl, Felix M.; Prather, Ben; Preciado-Lopez, Jorge A.; Pu, Hung-Yi; Ramakrishnan, Venkatessh; Rao, Ramprasad; Rawlings, Mark G.; Raymond, Alexander W.; Rezzolla, Luciano; Ricarte, Angelo; Ripperda, Bart; Roelofs, Freek; Rogers, Alan; Ros, Eduardo; Romero-Canizales, Cristina; Roshanineshat, Arash; Rottmann, Helge; Roy, Alan L.; Ruiz, Ignacio; Ruszczyk, Chet; Rygl, Kazi L. J.; Sanchez, Salvador; Sanchez-Arguelles, David; Sanchez-Portal, Miguel; Sasada, Mahito; Satapathy, Kaushik; Savolainen, Tuomas; Schloerb, F. Peter; Schonfeld, Jonathan; Schuster, Karl-Friedrich; Shao, Lijing; Shen, Zhiqiang; Small, Des; Sohn, Bong Won; SooHoo, Jason; Souccar, Kamal; Sun, He; Tazaki, Fumie; Tetarenko, Alexandra J.; Tiede, Paul; Tilanus, Remo P. J.; Titus, Michael; Torne, Pablo; Traianou, Efthalia; Trent, Tyler; Trippe, Sascha; Turk, Matthew; van Bemmel, Ilse; van Langevelde, Huib Jan; van Rossum, Daniel R.; Vos, Jesse; Wagner, Jan; Ward-Thompson, Derek; Wardle, John; Weintroub, Jonathan; Wex, Norbert; Wharton, Robert; Wielgus, Maciek; Wiik, Kaj; Witzel, Gunther; Wondrak, Michael F.; Wong, George N.; Wu, Qingwen; Yamaguchi, Paul; Yoon, Doosoo; Young, Andre; Young, Ken; Younsi, Ziri; Yuan, Feng; Yuan, Ye-Fei; Zensus, J. Anton; Zhang, Shuo; Zhao, Guang-Yao; Zhao, Shan-Shan; Ozel, Feryal; Agurto, Claudio; Allardi, Alexander; Amestica, Rodrigo; Araneda, Juan Pablo; Arriagada, Oriel; Berghuis, Jennie L.; Bertarini, Alessandra; Berthold, Ryan; Blanchard, Jay; Brown, Ken; Cardenas, Mauricio; Cantzler, Michael; Caro, Patricio; Castillo-Dominguez, Edgar; Chan, Tin Lok; Chang, Chih-Cheng; Chang, Dominic O.; Chang, Shu-Hao; Chang, Song-Chu; Chen, Chung-Chen; Chilson, Ryan; Chuter, Tim C.; Ciechanowicz, Miroslaw; Colin-Beltran, Edgar; Coulson, Iain M.; Crowley, Joseph; Degenaar, Nathalie; Dornbusch, Sven; Duran, Carlos A.; Everett, Wendeline B.; Faber, Aaron; Forster, Karl; Fuchs, Miriam M.; Gale, David M.; Geertsema, Gertie; Gonzalez, Edouard; Graham, Dave; Gueth, Frederic; Halverson, Nils W.; Han, Chih-Chiang; Han, Kuo-Chang; Hasegawa, Yutaka; Hernandez-Rebollar, Jose Luis; Herrera, Cristian; Herrero-Illana, Ruben; Heyminck, Stefan; Hirota, Akihiko; Hoge, James; Schimpf, Shelbi R. Hostler; Howie, Ryan E.; Huang, Yau-De; Jiang, Homin; Jinchi, Hao; John, David; Kimura, Kimihiro; Klein, Thomas; Kubo, Derek; Kuroda, John; Kwon, Caleb; Lacasse, Richard; Laing, Robert; Leitch, Erik M.; Li, Chao-Te; Liu, Ching-Tang; Liu, Kuan-Yu; Lin, Lupin C-C; Lu, Li-Ming; Mac-Auliffe, Felipe; Martin-Cocher, Pierre; Matulonis, Callie; Maute, John K.; Messias, Hugo; Meyer-Zhao, Zheng; Montana, Alfredo; Montenegro-Montes, Francisco; Montgomerie, William; Nolasco, Marcos Emir Moreno; Muders, Dirk; Nishioka, Hiroaki; Norton, Timothy J.; Nystrom, George; Ogawa, Hideo; Olivares, Rodrigo; Oshiro, Peter; Perez-Beaupuits, Juan Pablo; Parra, Rodrigo; Phillips, Neil M.; Poirier, Michael; Pradel, Nicolas; Qiu, Richard; Raffin, Philippe A.; Rahlin, Alexandra S.; Ramirez, Jorge; Ressler, Sean; Reynolds, Mark; Rodriguez-Montoya, Ivan; Saez-Madain, Alejandro F.; Santana, Jorge; Shaw, Paul; Shirkey, Leslie E., Jr.; Silva, Kevin M.; Snow, William; Sousa, Don; Sridharan, T. K.; Stahm, William; Stark, Anthony A.; Test, John; Torstensson, Karl; Venegas, Paulina; Walther, Craig; Wei, Ta-Shun; White, Chris; Wieching, Gundolf; Wijnands, Rudy; Wouterloot, Jan G. A.; Yu, Chen-Yu; Yu, Wei; Zeballos, Milagros; Event Horizon Telescope Collaboration., We present the first Event Horizon Telescope (EHT) observations of Sagittarius A* (Sgr A*), the Galactic center source associated with a supermassive black hole. These observations were conducted in 2017 using a global interferometric array of eight telescopes operating at a wavelength of λ = 1.3 mm. The EHT data resolve a compact emission region with intrahour variability. A variety of imaging and modeling analyses all support an image that is dominated by a bright, thick ring with a diameter of 51.8 ± 2.3 μas (68% credible interval). The ring has modest azimuthal brightness asymmetry and a comparatively dim interior. Using a large suite of numerical simulations, we demonstrate that the EHT images of Sgr A* are consistent with the expected appearance of a Kerr black hole with mass ∼4 × 106 M⊙, which is inferred to exist at this location based on previous infrared observations of individual stellar orbits, as well as maser proper-motion studies. Our model comparisons disfavor scenarios where the black hole is viewed at high inclination (i > 50°), as well as nonspinning black holes and those with retrograde accretion disks. Our results provide direct evidence for the presence of a supermassive black hole at the center of the Milky Way, and for the first time we connect the predictions from dynamical measurements of stellar orbits on scales of 103–105 gravitational radii to event-horizon-scale images and variability. Furthermore, a comparison with the EHT results for the supermassive black hole M87* shows consistency with the predictions of general relativity spanning over three orders of magnitude in central mass. © 2022. The Author(s). Published by the American Astronomical Society., The Event Horizon Telescope Collaboration thanks the following organizations and programs: the Academia Sinica; the Academy of Finland (projects 274477, 284495, 312496, 315721); the Agencia Nacional de Investigación y Desarrollo (ANID), Chile via NCN19_058 (TITANs) and Fondecyt 1221421, the Alexander von Humboldt Stiftung; an Alfred P. Sloan Research Fellowship; Allegro, the European ALMA Regional Centre node in the Netherlands, the NL astronomy research network NOVA and the astronomy institutes of the University of Amsterdam, Leiden University and Radboud University; the ALMA North America Development Fund; the Black Hole Initiative, which is funded by grants from the John Templeton Foundation and the Gordon and Betty Moore Foundation (although the opinions expressed in this work are those of the author(s) and do not necessarily reflect the views of these Foundations); Chandra DD7-18089X and TM6-17006X; the China Scholarship Council; China Postdoctoral Science Foundation fellowship (2020M671266); Consejo Nacional de Ciencia y Tecnología (CONACYT, Mexico, projects U0004-246083, U0004-259839, F0003-272050, M0037-279006, F0003-281692, 104497, 275201, 263356); the Consejería de Economía, Conocimiento, Empresas y Universidad of the Junta de Andalucía (grant P18-FR-1769), the Consejo Superior de Investigaciones Científicas (grant 2019AEP112); the Delaney Family via the Delaney Family John A. Wheeler Chair at Perimeter Institute; Dirección General de Asuntos del Personal Académico-Universidad Nacional Autónoma de México (DGAPA-UNAM, projects IN112417 and IN112820); the Dutch Organization for Scientific Research (NWO) VICI award (grant 639.043.513) and grant OCENW.KLEIN.113; the Dutch National Supercomputers, Cartesius and Snellius (NWO Grant 2021.013); the EACOA Fellowship awarded by the East Asia Core Observatories Association, which consists of the Academia Sinica Institute of Astronomy and Astrophysics, the National Astronomical Observatory of Japan, Center for Astronomical Mega-Science, Chinese Academy of Sciences, and the Korea Astronomy and Space Science Institute; the European Research Council (ERC) Synergy Grant "BlackHoleCam: Imaging the Event Horizon of Black Holes" (grant 610058); the European Union Horizon 2020 research and innovation programme under grant agreements RadioNet (No 730562) and M2FINDERS (No 101018682); the Generalitat Valenciana postdoctoral grant APOSTD/2018/177 and GenT Program (project CIDEGENT/2018/021); MICINN Research Project PID2019-108995GB-C22; the European Research Council for advanced grant "JETSET: Launching, propagation and emission of relativistic jets from binary mergers and across mass scales" (Grant No. 884631); the Institute for Advanced Study; the Istituto Nazionale di Fisica Nucleare (INFN) sezione di Napoli, iniziative specifiche TEONGRAV; the International Max Planck Research School for Astronomy and Astrophysics at the Universities of Bonn and Cologne; DFG research grant "Jet physics on horizon scales and beyond" (Grant No. FR 4069/2-1); Joint Princeton/Flatiron and Joint Columbia/Flatiron Postdoctoral Fellowships, research at the Flatiron Institute is supported by the Simons Foundation; the Japan Ministry of Education, Culture, Sports, Science and Technology (MEXT; grant JPMXP1020200109); the Japanese Government (Monbukagakusho: MEXT) Scholarship; the Japan Society for the Promotion of Science (JSPS) Grant-in-Aid for JSPS Research Fellowship (JP17J08829); the Joint Institute for Computational Fundamental Science, Japan; the Key Research Program of Frontier Sciences, Chinese Academy of Sciences (CAS, grants QYZDJ-SSW-SLH057, QYZDJSSW-SYS008, ZDBS-LY-SLH011); the Leverhulme Trust Early Career Research Fellowship; the Max-Planck-Gesellschaft (MPG); the Max Planck Partner Group of the MPG and the CAS; the MEXT/JSPS KAKENHI (grants 18KK0090, JP21H01137, JP18H03721, JP18K13594, 18K03709, JP19K14761, 18H01245, 25120007); the Malaysian Fundamental Research Grant Scheme (FRGS) FRGS/1/2019/STG02/UM/02/6; the MIT International Science and Technology Initiatives (MISTI) Funds; the Ministry of Science and Technology (MOST) of Taiwan (103-2119-M-001-010-MY2, 105-2112-M-001-025-MY3, 105-2119-M-001-042, 106-2112-M-001-011, 106-2119-M-001-013, 106-2119-M-001-027, 106-2923-M-001-005, 107-2119-M-001-017, 107-2119-M-001-020, 107-2119-M-001-041, 107-2119-M-110-005, 107-2923-M-001-009, 108-2112-M-001-048, 108-2112-M-001-051, 108-2923-M-001-002, 109-2112-M-001-025, 109-2124-M-001-005, 109-2923-M-001-001, 110-2112-M-003-007-MY2, 110-2112-M-001-033, 110-2124-M-001-007, and 110-2923-M-001-001); the Ministry of Education (MoE) of Taiwan Yushan Young Scholar Program; the Physics Division, National Center for Theoretical Sciences of Taiwan; the National Aeronautics and Space Administration (NASA, Fermi Guest Investigator grant 80NSSC20K1567, NASA Astrophysics Theory Program grant 80NSSC20K0527, NASA NuSTAR award 80NSSC20K0645); NASA Hubble Fellowship grant HST-HF2-51431.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555; the National Institute of Natural Sciences (NINS) of Japan; the National Key Research and Development Program of China (grant 2016YFA0400704, 2017YFA0402703, 2016YFA0400702); the National Science Foundation (NSF, grants AST-0096454, AST-0352953, AST-0521233, AST-0705062, AST-0905844, AST-0922984, AST-1126433, AST-1140030, DGE-1144085, AST-1207704, AST-1207730, AST-1207752, MRI-1228509, OPP-1248097, AST-1310896, AST-1440254, AST-1555365, AST-1614868, AST-1615796, AST-1715061, AST-1716327, AST-1716536, OISE-1743747, AST-1816420, AST-1935980, AST-2034306); NSF Astronomy and Astrophysics Postdoctoral Fellowship (AST-1903847); the Natural Science Foundation of China (grants 11650110427, 10625314, 11721303, 11725312, 11873028, 11933007, 11991052, 11991053, 12192220, 12192223); the Natural Sciences and Engineering Research Council of Canada (NSERC, including a Discovery Grant and the NSERC Alexander Graham Bell Canada Graduate Scholarships-Doctoral Program); the National Youth Thousand Talents Program of China; the National Research Foundation of Korea (the Global PhD Fellowship Grant: grants NRF-2015H1A2A1033752, the Korea Research Fellowship Program: NRF-2015H1D3A1066561, Brain Pool Program: 2019H1D3A1A01102564, Basic Research Support Grant 2019R1F1A1059721, 2021R1A6A3A01086420, 2022R1C1C1005255); Netherlands Research School for Astronomy (NOVA) Virtual Institute of Accretion (VIA) postdoctoral fellowships; Onsala Space Observatory (OSO) national infrastructure, for the provisioning of its facilities/observational support (OSO receives funding through the Swedish Research Council under grant 2017-00648); the Perimeter Institute for Theoretical Physics (research at Perimeter Institute is supported by the Government of Canada through the Department of Innovation, Science and Economic Development and by the Province of Ontario through the Ministry of Research, Innovation and Science); the Spanish Ministerio de Ciencia e Innovación (grants PGC2018-098915-B-C21, AYA2016-80889-P, PID2019-108995GB-C21, PID2020-117404GB-C21); the University of Pretoria for financial aid in the provision of the new Cluster Server nodes and SuperMicro (USA) for a SEEDING GRANT approved towards these nodes in 2020; the Shanghai Pilot Program for Basic Research, Chinese Academy of Science, Shanghai Branch (JCYJ-SHFY-2021-013); the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award for the Instituto de Astrofísica de Andalucía (SEV-2017- 0709); the Spinoza Prize SPI 78-409; the South African Research Chairs Initiative, through the South African Radio Astronomy Observatory (SARAO, grant ID 77948), which is a facility of the National Research Foundation (NRF), an agency of the Department of Science and Innovation (DSI) of South Africa; the Toray Science Foundation; Swedish Research Council (VR); the US Department of Energy (USDOE) through the Los Alamos National Laboratory (operated by Triad National Security, LLC, for the National Nuclear Security Administration of the USDOE (Contract 89233218CNA000001); and the YCAA Prize Postdoctoral Fellowship. APEX is a collaboration between the Max-Planck-Institut für Radioastronomie (Germany), ESO, and the Onsala Space Observatory (Sweden). The SMA is a joint project between the SAO and ASIAA and is funded by the Smithsonian Institution and the Academia Sinica. The JCMT is operated by the East Asian Observatory on behalf of the NAOJ, ASIAA, and KASI, as well as the Ministry of Finance of China, Chinese Academy of Sciences, and the National Key Research and Development Program (No. 2017YFA0402700) of China and Natural Science Foundation of China grant 11873028. Additional funding support for the JCMT is provided by the Science and Technologies Facility Council (UK) and participating universities in the UK and Canada. The LMT is a project operated by the Instituto Nacional de Astrófisica, Óptica, y Electrónica (Mexico) and the University of Massachusetts at Amherst (USA). The IRAM 30-m telescope on Pico Veleta, Spain is operated by IRAM and supported by CNRS (Centre National de la Recherche Scientifique, France), MPG (Max-Planck-Gesellschaft, Germany) and IGN (Instituto Geográfico Nacional, Spain). The SMT is operated by the Arizona Radio Observatory, a part of the Steward Observatory of the University of Arizona, with financial support of operations from the State of Arizona and financial support for instrumentation development from the NSF. Support for SPT participation in the EHT is provided by the National Science Foundation through award OPP-1852617 to the University of Chicago. Partial support is also provided by the Kavli Institute of Cosmological Physics at the University of Chicago. The SPT hydrogen maser was provided on loan from the GLT, courtesy of ASIAA. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), supported by NSF grant ACI-1548562, and CyVerse, supported by NSF grants DBI-0735191, DBI-1265383, and DBI-1743442. XSEDE Stampede2 resource at TACC was allocated through TG-AST170024 and TG-AST080026N. XSEDE JetStream resource at PTI and TACC was allocated through AST170028. This research is part of the Frontera computing project at the Texas Advanced Computing Center through the Frontera Large-Scale Community Partnerships allocation AST20023. Frontera is made possible by National Science Foundation award OAC-1818253. This research was carried out using resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy Office of Science. Additional work used ABACUS2.0, which is part of the eScience center at Southern Denmark University. Simulations were also performed on the SuperMUC cluster at the LRZ in Garching, on the LOEWE cluster in CSC in Frankfurt, on the HazelHen cluster at the HLRS in Stuttgart, and on the Pi2.0 and Siyuan Mark-I at Shanghai Jiao Tong University. The computer resources of the Finnish IT Center for Science (CSC) and the Finnish Computing Competence Infrastructure (FCCI) project are acknowledged. This research was enabled in part by support provided by Compute Ontario (http://computeontario.ca), Calcul Quebec (http://www.calculquebec.ca) and Compute Canada (http://www.computecanada.ca).
Published: 2022

35. Spatial-temporal analysis of COVID-19 cases in the state of Alagoas.

Author: Pereira-Júnior A, Silva L, Morais G, Sobrinho-Neto A, Oliveira D, Sá ML, Santos J, Messias HBG, Ferreira Júnior GC, Cavalcanti MGS, Lima BPS, Macêdo AC, Ribeiro MC, and Rocha TJM
Subjects: Brazil epidemiology, Humans, Retrospective Studies, Pandemics, SARS-CoV-2, COVID-19 epidemiology, Spatio-Temporal Analysis
Abstract: The COVID-19 pandemic has severely impacted Brazil, highlighting significant gaps in public health infrastructure. This study aims to analyze the spatial-temporal distribution of COVID-19 cases in Alagoas. The study covers all 102 municipalities in Alagoas, using official data from the Alagoas COVID-19 Panel. It is observational and retrospective with an ecological and quantitative approach. Data were collected up to July 2, 2022, totaling 305,806 cases. Spatial analysis was performed using R Statistical software, with Global Moran's Index (GMI) and Local Indicators of Spatial Association (LISAs) identifying spatial clusters. In 2020, municipalities showed significant but weak spatial autocorrelation (GMI = 0.2084; p < 0.05). High-High clusters appeared in Maceió and nearby municipalities. In 2021, spatial autocorrelation remained weak (GMI = 0.2344; p < 0.05). High-High clusters persisted in Satuba and Maceió, while Low-Low clusters expanded into northeastern Alagoas by 2022. The reduction in High-High clusters in Maceió in 2022 likely resulted from early vaccination efforts. The spatial distribution pattern of COVID-19 in Alagoas reveals significant insights into regional pandemic dynamics. Stable infection rates in the center-west and south of Alagoas may be due to lower population density and less movement. The dynamic nature of COVID-19 spread highlights the need for continuous monitoring and adaptive public health strategies. The study underscores the importance of targeted interventions and future research to refine spatial models and incorporate additional variables to enhance predictive accuracy and inform public health strategies.
Published: 2024
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36. Spindle epithelial tumor with thymus-like element (SETTLE)-Report of a rare thyroid carcinoma.

Author: Bernardo P, Messias H, Nogueira R, Lopes B, and Gomes P
Abstract: Spindle epithelial tumor with thymus-like element should be included in the differential diagnosis of thyroid gland cancers, particularly in medullary carcinoma, younger patients and indolent clinical presentation, because it may influence treatment and prognosis., Competing Interests: The authors declare to have no conflicts of interest in connection with this scientific work., (© 2024 The Author(s). Clinical Case Reports published by John Wiley & Sons Ltd.)
Published: 2024
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37. Knowledge, behavior and practices of the population during the pandemic against the transmission of SARS-CoV-2 in the state of Alagoas, Brazil.

Author: Carvalho Neto APM, Lisboa APS, Lemos Neto DA, Tavares MMA, Amaral MA, Moura MFS, Anjos TM, Omena ACS, Messias HBG, Omena BC, Ferreira Júnior GC, Cavalcanti MGS, Arinísio LS, Silva AC, Santos Júnior CJ, Oliveira ECT, Sales MLH, Ribeiro MC, and Rocha TJM
Subjects: Humans, Brazil epidemiology, Cross-Sectional Studies, Male, Adult, Female, Surveys and Questionnaires, Middle Aged, Young Adult, Pandemics prevention & control, Adolescent, Socioeconomic Factors, Social Media, Aged, COVID-19 prevention & control, COVID-19 transmission, COVID-19 epidemiology, Health Knowledge, Attitudes, Practice, SARS-CoV-2
Abstract: The World Health Organization (WHO) declared an international state of emergency in order to contain the rapid spread of COVID-19. To ensure that there is adherence to preventive measures by the population aimed at controlling the pandemic in Alagoas, it is expected that knowledge, behavior and practices play an important role in preventing and controlling the disease. In this sense, it becomes relevant to understand the knowledge of the population about the disease. To evaluate the knowledge, behavior and practices of social media users during social isolation to prevent the transmission of the SARS-CoV-2 in the state of Alagoas, Northeast, Brazil. A probabilistic sample was carried out across the entire territory of the state of Alagoas with those who have access to a device that accesses the internet and a cross-sectional study was carried out using an online questionnaire applied to a convenience sample, recruited between August 2021 and July 2022 by snowball sampling. The questionnaire consisted of seven sessions, the first collecting data on the socioeconomic and sociodemographic profile of the participants, and the other sessions involving knowledge, attitudes and practices, including topics related to the vaccination that had to be administered at that time. High popular knowledge about signs and symptoms, means of transmission and risk groups. Low knowledge about seeking health services. Based on the results obtained, information from official channels became relevant to better teach the population in order to reduce the impact of COVID-19.
Published: 2024
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38. Ectopic thyroid gland resembling a thyroglossal duct cyst.

Author: Messias H, Sequeira ML, Vilares M, Bitoque S, Rito M, and Gomes P
Abstract: Key Clinical Message: This rare diagnosis highlights the importance of anatomical and embryological knowledge in the differential diagnosis of neck masses., Abstract: A 41-year-old woman was referred to the head and neck surgery department because of a large midline neck mass at the level of the hyoid bone that was diagnostic for functioning thyroid tissue in a totally ectopic location., Competing Interests: The authors declare to have no conflicts of interest in connection with this scientific work., (© 2023 The Authors. Clinical Case Reports published by John Wiley & Sons Ltd.)
Published: 2023
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39. Pyramidal lobe-dominant papillary thyroid carcinoma-A rare entity with important clinical implications.

Author: Messias H, Sequeira ML, Nogueira R, Zagalo C, Martins M, and Gomes P
Abstract: Papillary thyroid carcinoma (PTC) primarily located in the pyramidal lobe of the thyroid gland is extremely rare, therefore the clinical and pathological features are not well understood. The authors describe a case of PTC of the pyramidal lobe, in a 77-year-old woman who underwent en bloc total thyroidectomy with pyramidal lobe, hyoid bone and cervical lymph node excision. In line with the present case, current literature reports a greater presence of worse prognostic factors, namely extrathyroidal extension, advanced T stage or presence of cervical lymph node metastasis. Recently, a new classification has been suggested-Upper Neck Papillary Thyroid Cancer (UPTC)-which encompasses these carcinomas, Delphi ganglion metastases and thyroglossal duct cyst carcinomas, with potential clinical and therapeutic implications, particularly the need for orthotopic thyroidectomy. Also, the complete excision of the pyramidal lobe during thyroidectomy may influence the success of radioactive iodine therapy and the patient's follow-up surveillance., Competing Interests: The authors declare to have no conflicts of interest in connection with this scientific work., (© 2023 The Authors. Clinical Case Reports published by John Wiley & Sons Ltd.)
Published: 2023
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40. A ring-like accretion structure in M87 connecting its black hole and jet.

Author: Lu RS, Asada K, Krichbaum TP, Park J, Tazaki F, Pu HY, Nakamura M, Lobanov A, Hada K, Akiyama K, Kim JY, Marti-Vidal I, Gómez JL, Kawashima T, Yuan F, Ros E, Alef W, Britzen S, Bremer M, Broderick AE, Doi A, Giovannini G, Giroletti M, Ho PTP, Honma M, Hughes DH, Inoue M, Jiang W, Kino M, Koyama S, Lindqvist M, Liu J, Marscher AP, Matsushita S, Nagai H, Rottmann H, Savolainen T, Schuster KF, Shen ZQ, de Vicente P, Walker RC, Yang H, Zensus JA, Algaba JC, Allardi A, Bach U, Berthold R, Bintley D, Byun DY, Casadio C, Chang SH, Chang CC, Chang SC, Chen CC, Chen MT, Chilson R, Chuter TC, Conway J, Crew GB, Dempsey JT, Dornbusch S, Faber A, Friberg P, García JG, Garrido MG, Han CC, Han KC, Hasegawa Y, Herrero-Illana R, Huang YD, Huang CL, Impellizzeri V, Jiang H, Jinchi H, Jung T, Kallunki J, Kirves P, Kimura K, Koay JY, Koch PM, Kramer C, Kraus A, Kubo D, Kuo CY, Li CT, Lin LC, Liu CT, Liu KY, Lo WP, Lu LM, MacDonald N, Martin-Cocher P, Messias H, Meyer-Zhao Z, Minter A, Nair DG, Nishioka H, Norton TJ, Nystrom G, Ogawa H, Oshiro P, Patel NA, Pen UL, Pidopryhora Y, Pradel N, Raffin PA, Rao R, Ruiz I, Sanchez S, Shaw P, Snow W, Sridharan TK, Srinivasan R, Tercero B, Torne P, Traianou E, Wagner J, Walther C, Wei TS, Yang J, and Yu CY
Abstract: The nearby radio galaxy M87 is a prime target for studying black hole accretion and jet formation 1,2 . Event Horizon Telescope observations of M87 in 2017, at a wavelength of 1.3 mm, revealed a ring-like structure, which was interpreted as gravitationally lensed emission around a central black hole 3 . Here we report images of M87 obtained in 2018, at a wavelength of 3.5 mm, showing that the compact radio core is spatially resolved. High-resolution imaging shows a ring-like structure of [Formula: see text] Schwarzschild radii in diameter, approximately 50% larger than that seen at 1.3 mm. The outer edge at 3.5 mm is also larger than that at 1.3 mm. This larger and thicker ring indicates a substantial contribution from the accretion flow with absorption effects, in addition to the gravitationally lensed ring-like emission. The images show that the edge-brightened jet connects to the accretion flow of the black hole. Close to the black hole, the emission profile of the jet-launching region is wider than the expected profile of a black-hole-driven jet, suggesting the possible presence of a wind associated with the accretion flow., (© 2023. The Author(s).)
Published: 2023
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41. Multifocal cutaneous angiosarcoma of the scalp-A challenging reconstructive case managed with skin substitutes.

Author: Messias H, Martins M, Zagalo C, and Gomes P
Subjects: Aged, Humans, Male, Scalp pathology, Scalp surgery, Hemangiosarcoma diagnosis, Hemangiosarcoma pathology, Hemangiosarcoma surgery, Skin Neoplasms diagnosis, Skin Neoplasms pathology, Skin Neoplasms surgery, Skin, Artificial
Abstract: Background: Cutaneous angiosarcoma (AS) of the head and neck is a rare highly aggressive tumor, often associated with difficult local control of the disease and poor prognosis. This article describes a case of multifocal cutaneous AS of the scalp, mainly addressing its difficult surgical management and challenging reconstruction and concludes with a review of the literature., Methods: A 70-year-old Caucasian male was referred to our hospital with a growing scalp lesion initially suspected to be benign, but later diagnosed with AS., Results: The patient had tumor recurrence and a difficult reconstruction for which dermal substitutes proved very useful., Conclusion: AS can mimic a benign lesion in its early stages. Skin substitutes, namely dermal templates, can be useful to meet the complex needs of reconstruction and oncological surveillance of patients with AS., (© 2022 The Authors. Cancer Reports published by Wiley Periodicals LLC.)
Published: 2022
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