[{"author":[{"last_name":"Mackenzie","first_name":"Ruari","full_name":"Mackenzie, Ruari"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"last_name":"Cantalupo","first_name":"Sebastiano","full_name":"Cantalupo, Sebastiano"},{"first_name":"Raffaella A","last_name":"Marino","full_name":"Marino, Raffaella A"},{"first_name":"Simon","last_name":"Lilly","full_name":"Lilly, Simon"},{"first_name":"Sowgat","last_name":"Muzahid","full_name":"Muzahid, Sowgat"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"full_name":"Schaye, Joop","last_name":"Schaye","first_name":"Joop"},{"last_name":"Wisotzki","first_name":"Lutz","full_name":"Wisotzki, Lutz"}],"acknowledgement":"The authors thank Daichi Kashino, for providing access to unpublished zCOSMOS Deep data, and Jakob S. den Brok for sharing code used in den Brok et al. (2020). GP and SC acknowledge the support of the Swiss National Science Foundation [grant PP00P2163824]. SM is supported by the Experienced Researchers Fellowship, Alexander von Humboldt-Stiftung, Germany. This work is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under the MUSE GTO programme. The major analysis and production of figures in this work was conducted in Python, using standard libraries which include NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), Matplotlib (Hunter 2007) and the interactive command shell IPython (Pérez & Granger 2007). This research also made use of Astropy, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), and Photutils, an Astropy package for detection and photometry of astronomica sources (Bradley et al. 2019). The python interface dustmaps (Green 2018) was used to query galactic extinction maps. topcat, a graphical tool for manipulating tabular data, was also utilized in this analysis (Taylor 2005). This research has made use of the \"Aladin sky atlas\" developed at CDS, Strasbourg Observatory, France (Bonnarel et al. 2000).","extern":"1","day":"01","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Oxford University Press","title":"Revealing the impact of quasar luminosity on giant Lyα nebulae","type":"journal_article","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","page":"494-509","date_created":"2022-07-07T10:11:15Z","quality_controlled":"1","volume":502,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","techniques: imaging spectroscopy","intergalactic medium","quasars: emission lines","quasars: general"],"external_id":{"arxiv":["2010.12589"]},"article_processing_charge":"No","article_type":"original","_id":"11526","abstract":[{"text":"We present the results from a MUSE survey of twelve z ≃ 3.15 quasars, which were selected to be much fainter (20 < iSDSS < 23) than in previous studies of giant Ly α nebulae around the brightest quasars (16.6 < iAB < 18.7). We detect H I Ly α nebulae around 100 per cent of our target quasars, with emission extending to scales of at least 60 physical kpc, and up to 190 pkpc. We explore correlations between properties of the nebulae and their host quasars, with the goal of connecting variations in the properties of the illuminating QSO to the response in nebular emission. We show that the surface brightness profiles of the nebulae are similar to those of nebulae around bright quasars, but with a lower normalization. Our targeted quasars are on average 3.7 mag (≃30 times) fainter in UV continuum than our bright reference sample, and yet the nebulae around them are only 4.3 times fainter in mean Ly α surface brightness, measured between 20 and 50 pkpc. We find significant correlations between the surface brightness of the nebula and the luminosity of the quasar in both UV continuum and Ly α. The latter can be interpreted as evidence for a substantial contribution from unresolved inner parts of the nebulae to the narrow components seen in the Ly α lines of some of our faint quasars, possibly from the inner circumgalactic medium or from the host galaxy’s interstellar medium.","lang":"eng"}],"arxiv":1,"issue":"1","date_updated":"2022-08-18T10:56:28Z","year":"2021","month":"03","status":"public","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"oa_version":"Preprint","date_published":"2021-03-01T00:00:00Z","doi":"10.1093/mnras/staa3277","publication_status":"published","intvolume":"       502","citation":{"short":"R. Mackenzie, G. Pezzulli, S. Cantalupo, R.A. Marino, S. Lilly, S. Muzahid, J.J. Matthee, J. Schaye, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 502 (2021) 494–509.","ieee":"R. Mackenzie <i>et al.</i>, “Revealing the impact of quasar luminosity on giant Lyα nebulae,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 502, no. 1. Oxford University Press, pp. 494–509, 2021.","ama":"Mackenzie R, Pezzulli G, Cantalupo S, et al. Revealing the impact of quasar luminosity on giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. 2021;502(1):494-509. doi:<a href=\"https://doi.org/10.1093/mnras/staa3277\">10.1093/mnras/staa3277</a>","ista":"Mackenzie R, Pezzulli G, Cantalupo S, Marino RA, Lilly S, Muzahid S, Matthee JJ, Schaye J, Wisotzki L. 2021. Revealing the impact of quasar luminosity on giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 502(1), 494–509.","mla":"Mackenzie, Ruari, et al. “Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 502, no. 1, Oxford University Press, 2021, pp. 494–509, doi:<a href=\"https://doi.org/10.1093/mnras/staa3277\">10.1093/mnras/staa3277</a>.","apa":"Mackenzie, R., Pezzulli, G., Cantalupo, S., Marino, R. A., Lilly, S., Muzahid, S., … Wisotzki, L. (2021). Revealing the impact of quasar luminosity on giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa3277\">https://doi.org/10.1093/mnras/staa3277</a>","chicago":"Mackenzie, Ruari, Gabriele Pezzulli, Sebastiano Cantalupo, Raffaella A Marino, Simon Lilly, Sowgat Muzahid, Jorryt J Matthee, Joop Schaye, and Lutz Wisotzki. “Revealing the Impact of Quasar Luminosity on Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2021. <a href=\"https://doi.org/10.1093/mnras/staa3277\">https://doi.org/10.1093/mnras/staa3277</a>."},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2010.12589"}],"scopus_import":"1"},{"issue":"2","arxiv":1,"abstract":[{"lang":"eng","text":"A prediction of the classic active galactic nucleus (AGN) unification model is the presence of ionization cones with different orientations depending on the AGN type. Confirmations of this model exist for present times, but it is less clear in the early Universe. Here, we use the morphology of giant Ly α nebulae around AGNs at redshift z ∼ 3 to probe AGN emission and therefore the validity of the AGN unification model at this redshift. We compare the spatial morphology of 19 nebulae previously found around type I AGNs with a new sample of four Ly α nebulae detected around type II AGNs. Using two independent techniques, we find that nebulae around type II AGNs are more asymmetric than around type I, at least at radial distances r > 30 physical kpc (pkpc) from the ionizing source. We conclude that the type I and type II AGNs in our sample show evidence of different surrounding ionizing geometries. This suggests that the classical AGN unification model is also valid for high-redshift sources. Finally, we discuss how the lack of asymmetry in the inner parts (r ≲ 30 pkpc) and the associated high values of the He II to Ly α ratios in these regions could indicate additional sources of (hard) ionizing radiation originating within or in proximity of the AGN host galaxies. This work demonstrates that the morphologies of giant Ly α nebulae can be used to understand and study the geometry of high-redshift AGNs on circumnuclear scales and it lays the foundation for future studies using much larger statistical samples."}],"date_updated":"2022-08-18T11:17:47Z","year":"2020","_id":"11530","status":"public","oa":1,"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"06","doi":"10.1093/mnras/staa1269","publication_status":"published","oa_version":"Preprint","date_published":"2020-06-01T00:00:00Z","scopus_import":"1","main_file_link":[{"url":"https://arxiv.org/abs/2005.01732","open_access":"1"}],"citation":{"chicago":"den Brok, J S, S Cantalupo, R Mackenzie, R A Marino, G Pezzulli, Jorryt J Matthee, S D Johnson, M Krumpe, T Urrutia, and W Kollatschny. “Probing the AGN Unification Model at Redshift z ∼ 3 with MUSE Observations of Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2020. <a href=\"https://doi.org/10.1093/mnras/staa1269\">https://doi.org/10.1093/mnras/staa1269</a>.","ista":"den Brok JS, Cantalupo S, Mackenzie R, Marino RA, Pezzulli G, Matthee JJ, Johnson SD, Krumpe M, Urrutia T, Kollatschny W. 2020. Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 495(2), 1874–1887.","apa":"den Brok, J. S., Cantalupo, S., Mackenzie, R., Marino, R. A., Pezzulli, G., Matthee, J. J., … Kollatschny, W. (2020). Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/staa1269\">https://doi.org/10.1093/mnras/staa1269</a>","mla":"den Brok, J. S., et al. “Probing the AGN Unification Model at Redshift z ∼ 3 with MUSE Observations of Giant Lyα Nebulae.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 495, no. 2, Oxford University Press, 2020, pp. 1874–87, doi:<a href=\"https://doi.org/10.1093/mnras/staa1269\">10.1093/mnras/staa1269</a>.","ama":"den Brok JS, Cantalupo S, Mackenzie R, et al. Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. <i>Monthly Notices of the Royal Astronomical Society</i>. 2020;495(2):1874-1887. doi:<a href=\"https://doi.org/10.1093/mnras/staa1269\">10.1093/mnras/staa1269</a>","ieee":"J. S. den Brok <i>et al.</i>, “Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 495, no. 2. Oxford University Press, pp. 1874–1887, 2020.","short":"J.S. den Brok, S. Cantalupo, R. Mackenzie, R.A. Marino, G. Pezzulli, J.J. Matthee, S.D. Johnson, M. Krumpe, T. Urrutia, W. Kollatschny, Monthly Notices of the Royal Astronomical Society 495 (2020) 1874–1887."},"intvolume":"       495","acknowledgement":"SC and GP gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. MK acknowledges support by DLR500R1904.","extern":"1","day":"01","author":[{"last_name":"den Brok","first_name":"J S","full_name":"den Brok, J S"},{"first_name":"S","last_name":"Cantalupo","full_name":"Cantalupo, S"},{"full_name":"Mackenzie, R","last_name":"Mackenzie","first_name":"R"},{"full_name":"Marino, R A","last_name":"Marino","first_name":"R A"},{"full_name":"Pezzulli, G","first_name":"G","last_name":"Pezzulli"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Johnson","first_name":"S D","full_name":"Johnson, S D"},{"last_name":"Krumpe","first_name":"M","full_name":"Krumpe, M"},{"full_name":"Urrutia, T","first_name":"T","last_name":"Urrutia"},{"full_name":"Kollatschny, W","last_name":"Kollatschny","first_name":"W"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Oxford University Press","title":"Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae","publication":"Monthly Notices of the Royal Astronomical Society","page":"1874-1887","date_created":"2022-07-07T10:40:17Z","type":"journal_article","language":[{"iso":"eng"}],"article_type":"original","article_processing_charge":"No","quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","intergalactic medium","quasars: emission lines","quasars: general"],"volume":495,"external_id":{"arxiv":["2005.01732"]}},{"status":"public","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"month":"11","arxiv":1,"abstract":[{"lang":"eng","text":"While traditionally associated with active galactic nuclei (AGN), the properties of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549, 1551 Å) emission lines are still uncertain as large, unbiased samples of sources are scarce. We present the first blind, statistical study of C II], C III] and C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17 C IV emitters, whose nature we investigate using optical colours as well as Hubble Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7 C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4) star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like morphologies. Bright C II] emitters have individual X-ray detections as well as high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a variety of optical morphologies, including isolated and interacting galaxies and low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young, blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts and large BHAR (0.8  M⊙ yr−1). We also find some surprising C II], C III] and C IV emitters with rest-frame equivalent widths (EWs) that could be as large as 50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the line-emitting regions may explain the large EW. These bright C II], C III] and C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil their nature."}],"issue":"3","date_updated":"2022-08-19T07:59:57Z","year":"2017","_id":"11566","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1703.10169"}],"intvolume":"       471","citation":{"ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2558-2574. doi:<a href=\"https://doi.org/10.1093/mnras/stx1712\">10.1093/mnras/stx1712</a>","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.","short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2558–2574.","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press, 2017, pp. 2558–74, doi:<a href=\"https://doi.org/10.1093/mnras/stx1712\">10.1093/mnras/stx1712</a>.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1712\">https://doi.org/10.1093/mnras/stx1712</a>","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1712\">https://doi.org/10.1093/mnras/stx1712</a>."},"doi":"10.1093/mnras/stx1712","publication_status":"published","oa_version":"Preprint","date_published":"2017-11-01T00:00:00Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Oxford University Press","title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ","acknowledgement":"We would like to thank the anonymous referee for her/his valuable input that helped improve the clarity and interpretation of our results. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO), through a Veni fellowship. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data are based on observations made with the Isaac Newton Telescope (proposals 13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. Also based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and J. Schombert for their cosmology calculator. We would like to thank the authors of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages publicly available. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is ","extern":"1","day":"01","author":[{"first_name":"Andra","last_name":"Stroe","full_name":"Stroe, Andra"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee"},{"last_name":"Calhau","first_name":"João","full_name":"Calhau, João"},{"full_name":"Oteo, Ivan","last_name":"Oteo","first_name":"Ivan"}],"article_processing_charge":"No","article_type":"original","volume":471,"quality_controlled":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","quasars: emission lines","galaxies: star formation","cosmology: observations"],"external_id":{"arxiv":["1703.10169"]},"publication":"Monthly Notices of the Royal Astronomical Society","page":"2558-2574","date_created":"2022-07-12T12:33:16Z","type":"journal_article","language":[{"iso":"eng"}]},{"doi":"10.1093/mnras/stx1713","publication_status":"published","date_published":"2017-11-01T00:00:00Z","oa_version":"Preprint","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1703.10169"}],"citation":{"chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1713\">https://doi.org/10.1093/mnras/stx1713</a>.","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1713\">https://doi.org/10.1093/mnras/stx1713</a>","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3), 2575–2586.","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press, 2017, pp. 2575–86, doi:<a href=\"https://doi.org/10.1093/mnras/stx1713\">10.1093/mnras/stx1713</a>.","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.","ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2575-2586. doi:<a href=\"https://doi.org/10.1093/mnras/stx1713\">10.1093/mnras/stx1713</a>","short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2575–2586."},"intvolume":"       471","year":"2017","issue":"3","abstract":[{"text":"Recently, the C III] and C IV emission lines have been observed in galaxies in the early Universe (z > 5), providing new ways to measure their redshift and study their stellar populations and active galactic nuclei (AGN). We explore the first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively) presented in Stroe et al. (2017). We derive luminosity functions (LF) and study properties of C II], C III] and C IV line emitters through comparisons to the LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity. The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast, the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that the brightest UV sources (MUV < −22) will universally have C III] and C IV emission. However, on average, C III] and C IV are not as abundant as H α or Ly α emitters at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1 to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly competitive in confirming high-redshift candidates when the hosts are intrinsically bright and the effective Ly α escape fraction is below 1 per cent. While C III] and C IV were proposed as good tracers of young, relatively low-metallicity galaxies typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively hosted by AGN/quasars, especially at large line equivalent widths.","lang":"eng"}],"arxiv":1,"date_updated":"2022-08-19T08:02:04Z","_id":"11567","oa":1,"publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"status":"public","month":"11","publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2022-07-12T12:54:57Z","page":"2575-2586","language":[{"iso":"eng"}],"type":"journal_article","article_type":"original","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high redshift","galaxies: luminosity function","mass function","quasars: emission lines","star formation","cosmology: observations"],"quality_controlled":"1","volume":471,"external_id":{"arxiv":["1703.10169"]},"extern":"1","day":"01","author":[{"full_name":"Stroe, Andra","first_name":"Andra","last_name":"Stroe"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J"},{"full_name":"Calhau, João","last_name":"Calhau","first_name":"João"},{"first_name":"Ivan","last_name":"Oteo","full_name":"Oteo, Ivan"}],"title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publisher":"Oxford University Press"}]