Prime Focus Spectrograph (PFS) for the Subaru telescope: overview, recent progress, and future perspectives

Tamura, Naoyuki; Takato, Naruhisa; Shimono, Atsushi; Moritani, Yuki; Yabe, Kiyoto; Ishizuka, Yuki; Ueda, Akitoshi; Kamata, Yukiko; Aghazarian, Hrand; Arnouts, S.; Barban, Gabriel; Barkhouser, Robert H.; Borges, Renato C.; Braun, David; Carr, Michael; Chabaud, Pierre-Yves; Chang, Yin-Chang; Chen, Hsin-Yo; Chiba, Masashi; Chou, Richard C. Y.; Chu, You‐Hua; Cohen, Judith G.; Almeida, Rodrigo P. de; Oliveira, Antônio César de; Oliveira, Lígia Souza de; Dekany, Richard; Dohlen, Kjetil; Santos, Jesulino Bispo dos; Santos, Leandro Henrique dos; Ellis, Richard S.; Fabricius, Maximilian; Ferrand, Didier; Ferreira, Décio; Golebiowski, Mirek; Greene, Jenny E.; Größ, Johannes; Gunn, James E.; Hammond, Randolph P.; Harding, Albert; Hart, Murdock; Heckman, Timothy M.; Hirata, Christopher M.; Ho, P. T. P.; Hope, Stephen C.; Hovland, Larry E.; Hsu, Shu-Fu; Hu, Yen-Shan; Huang, Pingjie; Jaquet, M.; Jing, Y. P.; Karr, J.; Kimura, Masahiko; King, Matthew E.; Komatsu, Eiichiro; Brun, V. Le; Fèvre, O. Le; Fur, Arnaud Le; Mignant, D. Le; Ling, Hung-Hsu; Loomis, Craig; Lupton, Robert H.; Madec, F.; Mao, Peter H.; Marrara, Lucas Souza; Oliveira, C. Mendes de; Minowa, Yosuke; Morantz, Chaz; Murayama, Hitoshi; Murray, Graham J.; Ohyama, Youichi; Orndorff, Joseph; Pascal, Sandrine; Pereira, Jefferson M.; Reiley, Daniel J.; Reinecke, M.; Ritter, Andreas; Roberts, Mitsuko; Schwochert, Mark A.; Seiffert, M. D.; Smee, Stephen A.; Sodré, L.; Spergel, David N.; Steinkraus, Aaron J.; Strauss, Michael A.; Surace, C.; Suto, Yasushi; Suzuki, N.; Swinbank, J.; Tait, Philip J.; Takada, Masahiro; Tamura, Takuya; Tanaka, Yôko; Tresse, L.; Verducci, Orlando; Vibert, D.; Vidal, Clément; Wang, Shiang‐Yu; Wen, C. Y.; Yan, Chi-Hung; Yasuda, Naoki

doi:10.1117/12.2232103

Cited by 95 publications

(41 citation statements)

References 17 publications

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“…By combining weak lensing measurements, on-going surveys such as Subaru/Primary Spectroscopic Survey (Sugai et al 2012(Sugai et al , 2014Tamura et al 2016) would certainly benefit us for investigating a three dimensional matter distribution in the local Universe to the Cold Spot. Figure 4.…”

Section: Discussionmentioning

confidence: 99%

“…One of such anomalies is the CMB Cold Spot centred at (l, b) = (209 • , −57 • ) with a temperature decrement ∆T ∼ −100µK surrounded by a hot ring (Vielva et al 2004;Cruz et al 2005;Planck Collaboration et al 2014, 2016. Although a seemingly peculiar 'cold' spot within ∼ 7 • from the center is not significant, a structure of the 'cold' spot surrounded by a hot ring within ∼ 20 • is significant at 3σ assuming that the CMB temperature fluctuation is isotropic Gaussian (Cruz et al 2005;Zhang & Huterer 2010;Inoue et al 2010;Nadathur et al 2014).…”

Section: Introductionmentioning

confidence: 99%

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Probing supervoids with weak lensing

Higuchi

Inoue

2018

Monthly Notices of the Royal Astronomical Society

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The cosmic microwave background (CMB) has non-Gaussian features in the temperature fluctuations. An anomalous cold spot surrounded with a hot ring, called the Cold Spot is one of such features. If a large underdence region (supervoid) resides towards the Cold Spot, we would be able to detect a systematic shape distortion in the images of background source galaxies via weak lensing effect. In order to estimate the detectability of such signals, we used the data of N-body simulations to simulate full-sky ray-tracing of source galaxies. We searched for a most prominent underdense region using the simulated convergence maps smoothed at a scale of 20 degree and obtained tangential shears around it. The lensing signal expected in a concordant ΛCDM model can be detected at a signal-to-noise ratio S/N ∼ 3. If a supervoid with a radius of ∼ 200 h −1 Mpc and a density contrast δ 0 ∼ −0.3 at the centre resides at a redshift z ∼ 0.2, on-going and near-future weak gravitational lensing surveys would detect a lensing signal with S/N 4 without resorting to stacking. From the tangential shear profile, we can obtain a constraint on the projected mass distribution of the supervoid.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Probing supervoids with weak lensing

Higuchi

Inoue

2018

Monthly Notices of the Royal Astronomical Society

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“…Future work will be needed to understand such selection biases and categorise individual protoclusters with, e.g., X-ray properties (Gobat et al 2011;Valentino et al 2016;Wang et al 2016) and Hi tomography (Lee et al 2016). The upcoming eROSITA (Merloni et al 2012), a successor to the ASTRO-H (Hitomi, Takahashi et al 2016), and the Prime Focus Spectrograph on the Subaru Telescope (Tamura et al 2016) will possess the exceptional capability needed to reveal these unique objects.…”

Section: Future Prospects: Diverse Protoclustersmentioning

confidence: 99%

MAHALO Deep Cluster Survey II. Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2

Shimakawa

Koyama

Röttgering

et al. 2018

Monthly Notices of the Royal Astronomical Society

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This paper is the second in a series presenting the results of our deep Hα-line survey towards protoclusters at z > 2, based on narrow-band imaging with the Subaru Telescope. This work investigates massive galaxies in a protocluster region associated with a radio galaxy (PKS 1138−262), the Spiderweb galaxy, at z = 2.2. Our 0.5 mag deeper narrow-band imaging than previous surveys collects a total of 68 Hα emitters (HAE). 17 out of the 68 are newly discovered protocluster members. First, a very high characteristic stellar mass of M * = 10 11.73 M is measured from a Schechter function fit to the mass distribution of HAEs. Together with the Chandra X-ray data, we find that four out of six massive HAEs (M > 10 11 M ) show bright X-ray emission, suggesting that they host active galactic nuclei (AGNs). Their mass estimates, therefore, would be affected by the nuclear emission from AGNs. Notably, the X-ray detected HAEs are likely positioned near the boundary between star-forming and quiescent populations in the rest-frame UV J plane. Moreover, our deep narrow-band data succeed in probing the bright Hα (+[Nii]) line nebula of the Spiderweb galaxy extending over ∼ 100 physical kpc. These results suggest that the massive galaxies in the Spiderweb protocluster are on the way to becoming the bright red sequence objects seen in local galaxy clusters, where AGNs might play an essential role in their quenching processes. Though a more statistical database is needed to build a general picture.

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“…With spectroscopic sky surveys pushing to higher redshift and fainter luminosities (e.g., SDSS: York et al 2000; DESI: Levi et al 2013;PFS: Takada et al 2014;Tamura et al 2016), the need for a good classification diagram for emission line galaxies at higher redshift is compelling. Some efforts have been made to develop diagnostic diagrams with spectral features in a narrower wavelength range.…”

Section: Introductionmentioning

confidence: 99%

A New Diagnostic Diagram of Ionization Sources for High-redshift Emission Line Galaxies

Zhang

Hao

2018

ApJ

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We propose a new diagram, the kinematics-excitation (KEx) diagram, which uses the [O III] λ5007/Hβ line ratio and the [O III] λ5007emission line width (σ [O III] ) to diagnose the ionization source and physical properties of active galactic nuclei (AGNs) and star-forming galaxies (SFGs). The KEx diagram is a suitable tool to classify emission line galaxies at intermediate redshift because it uses only the [O III] λ5007 and Hβ emission lines. We use the main galaxy sample of SDSS DR7 and the Baldwin−Phillips−Terlevich (BPT) diagnostic to calibrate the diagram at low redshift. The diagram can be divided into three regions: the KEx-AGN region, which consists mainly of pure AGNs, the KEx-composite region, which is dominated by composite galaxies, and the KEx-SFG region, which contains mostly SFGs. LINERs strongly overlap with the composite and AGN regions. AGNs are separated from SFGs in this diagram mainly because they preferentially reside in luminous and massive galaxies and have higher [O III]/Hβ than SFGs. The separation between AGNs and SFGs is even cleaner thanks to the additional 0.15/0.12dex offset in σ [O III] at fixed luminosity/stellar mass. We apply the KEx diagram to 7866 galaxies at 0.3<z<1 in the DEEP2 Galaxy Redshift Survey, and compare it to an independent X-ray classification scheme using Chandra observations. X-ray AGNs are mostly located in the KEx-AGN region, while X-ray SFGs are mostly located in the KEx-SFG region. Almost all Type 1 AGNs lie in the KEx-AGN region. These tests support the reliability of this classification diagram for emission line galaxies at intermediate redshift.At z∼2, the demarcation line between SFGs and AGNs is shifted by ∼0.3dex toward higher values of σ [O III] due to evolution effects.

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Prime Focus Spectrograph (PFS) for the Subaru telescope: overview, recent progress, and future perspectives

Cited by 95 publications

References 17 publications

Probing supervoids with weak lensing

Probing supervoids with weak lensing

MAHALO Deep Cluster Survey II. Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2

A New Diagnostic Diagram of Ionization Sources for High-redshift Emission Line Galaxies

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