![[C ii] to FIR luminosity ratio as a function of FIR luminosity for our HSC quasars (cyan stars; both the Cycle 4 and 5 samples are included): this is an updated version from the figure presented in Izumi et al. (2018b). Compilations of various kinds of galaxies from the literature are also plotted: local LIRGs (Díaz-Santos et al. 2013), local ULIRGs (Farrah et al. 2013), $z \gt 2$ FIR- or UV-luminous galaxies (Maiolino et al. 2009; Ivison et al. 2010; De Breuck et al. 2011; Wagg et al. 2012; Riechers et al. 2013; Gullberg et al. 2015; Capak et al. 2015), and $z \gtrsim 6$ quasars (Maiolino et al. 2005; Venemans et al. 2012, 2016, 2017a, 2017c, 2018; Wang et al. 2013, 2016; Willott et al. 2013, 2015, 2017; Bañados et al. 2015; Shao et al. 2017; Decarli et al. 2017, 2018; Mazzucchelli et al. 2017). For all quasar samples, we assumed a graybody spectrum with $T_d = 47$ K and $\beta = 1.6$ to calculate $L_{\rm FIR}$, in order to maintain consistency. The horizontal dashed line indicates the Milky Way value ($\sim 3 \times 10^{-3}$; Carilli & Walter 2013). Where necessary, TIR luminosity was converted to FIR luminosity using $L_{\rm TIR} \simeq 1.3 L_{\rm FIR}$ (Carilli & Walter 2013). The diagonal dotted line indicates our best fit to the quasar data, excluding objects with upper and/or lower limits. (Color online)](https://oup.silverchair-cdn.com/oup/backfile/Content_public/Journal/pasj/71/6/10.1093_pasj_psz096/2/pasj_71_6_111_f13.jpeg?Expires=1749862725&Signature=NPgv3XKUVe28m5YeItSANDz5yuD9CYLGAuFM1bonxSfoJVU-qrUaXQjXsRughRmRMFBB7jTJYUQyq0rabpolnOCiI4ZbXwsrlatSpTSViLDnEP6NXk5mTiTxfMHPn~96aYueu2kE2spTCVcZG-Draf9zQ1tLbc5a1VXm1GOR~p~Pb2LMzXmv1X4Fw--zpy5bTKlckp5qKXNsu8anuvglOWxMg9DY~mrjQ~y7WOBcr11I3c-yQKBqWOECLL0Ow33Ltn4P-qaKJq7qKrik-WGOOhqirYEfeRrDnsvJ7gIyPtFOkhLF-tZuCv4dTdXbtWriaPIqszoGoVtPYIXPYLcclA__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
[C ii] to FIR luminosity ratio as a function of FIR luminosity for our HSC quasars (cyan stars; both the Cycle 4 and 5 samples are included): this is an updated version from the figure presented in Izumi et al. (2018b). Compilations of various kinds of galaxies from the literature are also plotted: local LIRGs (Díaz-Santos et al. 2013), local ULIRGs (Farrah et al. 2013), |$z \gt 2$| FIR- or UV-luminous galaxies (Maiolino et al. 2009; Ivison et al. 2010; De Breuck et al. 2011; Wagg et al. 2012; Riechers et al. 2013; Gullberg et al. 2015; Capak et al. 2015), and |$z \gtrsim 6$| quasars (Maiolino et al. 2005; Venemans et al. 2012, 2016, 2017a, 2017c, 2018; Wang et al. 2013, 2016; Willott et al. 2013, 2015, 2017; Bañados et al. 2015; Shao et al. 2017; Decarli et al. 2017, 2018; Mazzucchelli et al. 2017). For all quasar samples, we assumed a graybody spectrum with |$T_d = 47$| K and |$\beta = 1.6$| to calculate |$L_{\rm FIR}$|, in order to maintain consistency. The horizontal dashed line indicates the Milky Way value (|$\sim 3 \times 10^{-3}$|; Carilli & Walter 2013). Where necessary, TIR luminosity was converted to FIR luminosity using |$L_{\rm TIR} \simeq 1.3 L_{\rm FIR}$| (Carilli & Walter 2013). The diagonal dotted line indicates our best fit to the quasar data, excluding objects with upper and/or lower limits. (Color online)
