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We adopt the sample of SALGs from the SCUBA ΗΔΗ Degree. Extragalactic Survey (SILADIESAlortieretal.2005:Coppinetal.2006) as described in Section 2. | We adopt the sample of SMGs from the SCUBA HAlf Degree Extragalactic Survey \citep[SHADES --][]{2005MNRAS.363..563M,2006MNRAS.372.1621C} as described in Section 2. |
In Section 3. we investigate tvpical optical/NIIU colours of the racio-detected: SMCGs. | In Section 3, we investigate typical optical/NIR colours of the radio-detected SMGs. |
. We apply our direct. identification method for radio-undetected SMCs in Section 4. | We apply our direct identification method for radio-undetected SMGs in Section 4. |
We then discuss a possible evolutionary link. between SALGs and 3zixs in Section 5. | We then discuss a possible evolutionary link between SMGs and BzKs in Section 5. |
Finally we give our summary in Section 6. | Finally we give our summary in Section 6. |
Vhroughout this paper. we assume a cosmology with OQ,=03. O4=0.7 and fy= TOkmsee Alpe + ΑΙ | Throughout this paper, we assume a cosmology with $\Omega_\mathrm{m} =0.3$, $\Omega_\Lambda =0.7$ and $H_0 =70$$\,$ $\,$ $^{-1}$$\,$ $^{-1}$. |
magnitudes in this paper use the AB svstem unless ofherwise noted. | All magnitudes in this paper use the AB system unless otherwise noted. |
The sample of SALGs is taken from the SILADES source catalogue in the Subaru/NMM-Newton Deep Field (SNDIE). which contains GO reliable sources (Coppinetal.2006).. | The sample of SMGs is taken from the SHADES source catalogue in the Subaru/XMM-Newton Deep Field (SXDF), which contains 60 reliable sources \citep{2006MNRAS.372.1621C}. |
Ivisonetal.(2007). found robust 41 radio associations for 35 SALGs. | \cite{2007MNRAS.380..199I} found robust 41 radio associations for 35 SMGs. |
They. caleulatecl the formal. significance of cach of the potential submim/radio associations. by correcting the raw Poisson probability with the method of Downesetal.(1986)... | They calculated the formal significance of each of the potential submm/radio associations, by correcting the raw Poisson probability with the method of \cite{1986MNRAS.218...31D}. |
A subnimyracdio association is regarded: as being robust if the corrected. Poisson probability 2% is less than 0.05 with a search radius of 8”. | A submm/radio association is regarded as being robust if the corrected Poisson probability $P'$ is less than 0.05 with a search radius of $''$. |
Phe detection limit at GGllz is yely beam+ in the best region (La: vison et al. | The detection limit at GHz is $\mu$ Jy $^{-1}$ in the best region $\sigma$; Ivison et al. |
2007) with a EWIIM of 1.7". | 2007) with a FWHM of $''$. |
One of the SALGs. SADES5O.6. has a triple radio association. 2 robust and 1 tentative. | One of the SMGs, SXDF850.6, has a triple radio association, 2 robust and 1 tentative. |
X high angular resolution image with Submillimetre Array (SALA) pinned down the tentative radio association as a rue racio counterpart (J. Dunlop et ab. | A high angular resolution image with Submillimetre Array (SMA) pinned down the tentative radio association as a true radio counterpart (J. Dunlop et al., |
private communication) | private communication). |
Thus. two "robust radio associations happen by chance. | Thus, two `robust' radio associations happen by chance. |
Exclucing these two chance associations. and adding the true radio counterpart. of SADESSO.G. we investigate 40 radio associations in total. | Excluding these two chance associations, and adding the true radio counterpart of SXDF850.6, we investigate 40 radio associations in total. |
Ivisonetal.(2007) also suggest one jii source as a counterpart οSNDES5SO.7 1. which has no radio associations. | \cite{2007MNRAS.380..199I} also suggest one $\mu$ m source as a counterpart of SXDF850.71, which has no radio associations. |
We also include this MIS counterpart in the analvsis below. | We also include this MIR counterpart in the analysis below. |
However. this source is eventually excluded in our study. since we find no reliable A;- band counterpart within a search radius of 2". | However, this source is eventually excluded in our study, since we find no reliable $K_s$ -band counterpart within a search radius of $''$. |
We search for optical anc NIU counterparts of 40. radio and 1 MI sources with a search. radius of 2". using the ollicial optical source catalogue of SNDS (ver.1.Furusawaetal.2008). and the NI source catalogue of UIXIDSS data release 2. | We search for optical and NIR counterparts of 40 radio and 1 MIR sources with a search radius of $''$, using the official optical source catalogue of SXDS \citep[ver.\,1 --][]{2008arXiv0801.4017F} and the NIR source catalogue of UKIDSS data release 2. |
Here. we concentrate on the sources detected in the A, band only. | Here we concentrate on the sources detected in the $K_s$ band only. |
The detection limits in the JJ and A, bands are 22.61 and mmae (5oinVega:Warrenetal. 2007).. respectively. | The detection limits in the $J$ and $K_s$ bands are 22.61 and mag \citep[5\,$\sigma$ in Vega;][]{2007MNRAS.375..213W}, respectively. |
In the case of a multiple association [or à radio source. we adopt the closest A;-band source to the radio position as the correct. optical-NITU counterpart. | In the case of a multiple association for a radio source, we adopt the closest $K_s$ -band source to the radio position as the correct optical-NIR counterpart. |
Some optical counterparts from the SANDS catalogue. are [ound to be different from the NI. counterparts. (niostlIv due to confusion of optical sources). | Some optical counterparts from the SXDS catalogue are found to be different from the NIR counterparts (mostly due to confusion of optical sources). |
In this case. we perform aperture photometry at the position of NLR sources. | In this case, we perform aperture photometry at the position of NIR sources. |
We use matched aperture photometry with a H inmeter to determine colours. | We use matched aperture photometry with a $''$ diameter to determine colours. |
However. when single A.- magnitudes. are quoted. they are total magnitudes (Petrosian. magnitudes in the νο catalogue). | However, when single $K_s$ -band magnitudes are quoted they are total magnitudes (Petrosian magnitudes in the UKIDSS catalogue). |
We correct optical photometry for the galactic cirrus absorption. | We correct optical photometry for the galactic cirrus absorption. |
We note that SNDESDO0.21 is obviously à nearby galaxy with a large angular size. ~30". | We note that SXDF850.21 is obviously a nearby galaxy with a large angular size, $\sim 30''$. |
For this galaxy. we measure optical/NIIS colours from total magnitudes. | For this galaxy, we measure optical/NIR colours from total magnitudes. |
Using the UKIDSS/UDS catalogue. we Lined A.-banc counterparts for 29. radio sources out of 40. | Using the UKIDSS/UDS catalogue, we find $K_s$ -band counterparts for 29 radio sources out of 40. |
For SADES50.6 (with the SALA identification)) we find a νοband counterpart at 0.19" away from the radio position. but we find no optical counterpart. although it is very close to an optical source ~1.5” away. | For SXDF850.6 (with the SMA identification), we find a $K_s$ -band counterpart at $''$ away from the radio position, but we find no optical counterpart, although it is very close to an optical source $\sim1.5''$ away. |
This case is similar to three other SMGs discussed in Smail et al.(2004 sce their Figure 3). | This case is similar to three other SMGs discussed in Smail et al.(2004 – see their Figure 3). |
Excluding this complicated case. we obtain opticalNIR photometry of 28 radio counterparts for 24 SILXDISS sources in the SNDE. | Excluding this complicated case, we obtain optical–NIR photometry of 28 radio counterparts for 24 SHADES sources in the SXDF. |
No A.-band source is found at the position of the ΑΔΗ counterpart. of SXDESDQO.71. | No $K_s$ -band source is found at the position of the MIR counterpart of SXDF850.71. |
Out of the 28 ÁAN.-detected: radio sources. 20 are singlv associated: with the SILADES sources (hereafter singlv associated SALCGs). | Out of the 28 $K_s$ -detected radio sources, 20 are singly associated with the SHADES sources (hereafter singly associated SMGs). |
Fie. | Fig. |
7 shows the radial density profile for Ποιά galaxies selected. as discussed. in 6??.. taking into account the area masked bv the colour-selected: cluster. galaxies. (3.0 arcmün in total out of the 27.5 arcmin central field). | \ref{fig-depletion} shows the radial density profile for field galaxies selected as discussed in $\S$ \ref{sec-colmag}, taking into account the area masked by the colour-selected cluster galaxies (3.0 $^2$ in total out of the 27.5 $^2$ central field). |
We utilize both [lanking fields in order to determine the anlensed surface number density of the red population to be | We utilize both flanking fields in order to determine the unlensed surface number density of the red population to be. |
With no colour selection this density rises to np —43.2 ο which gives some indication of the likelihood that non-cluster galaxies might be cliscarelect via this colour cut. | With no colour selection this density rises to $n_T$ =43.2 $^{-2}$ which gives some indication of the likelihood that non-cluster galaxies might be discarded via this colour cut. |
Fie. | Fig. |
7 gives a clear detection of the depletion signal at the 37 level within a diameter of ~SO aresec (7350 kpc or h=0.5. gq,= 0.5). | \ref{fig-depletion} gives a clear detection of the depletion signal at the $\sigma$ level within a diameter of $\sim$ 80 arcsec $\sim$ 350 kpc for $h=0.5$, $q_o=0.5$ ). |
However. its absolute significance depends critically on the adopted: value of no. | However, its absolute significance depends critically on the adopted value of $n_0$. |
We estimate he uncertainty in our measurement of no (indicated bv the dashed. lines in Fig. 7)) | We estimate the uncertainty in our measurement of $n_0$ (indicated by the dashed lines in Fig. \ref{fig-depletion}) ) |
using the dispersion in counts in he full Z£-band dataset shown in Fig. 2.. | using the dispersion in counts in the full $H$ -band dataset shown in Fig. \ref{fig-fov}. |
Phe elfects of this uncertainty are discussed further in $77. | The effects of this uncertainty are discussed further in $\S\ref{sec-err}$. |
‘To investigate the magnitude and. significance of this possible depletion. we adopted. a maximum likelihood approach based on that developed. by Schneider. Wing Erben (2000: hereafter. SIE). | To investigate the magnitude and significance of this possible depletion, we adopted a maximum likelihood approach based on that developed by Schneider, King Erben (2000; hereafter SKE). |
In this formulation. which avoids the loss of information induced by the racial binning (as in Fig. 7)). | In this formulation, which avoids the loss of information induced by the radial binning (as in Fig. \ref{fig-depletion}) ), |
the log-likelihood equation takes the form: where ny is the unlensed number density of background galaxies 7). pris the magnification. 6; is the position vector of the ith. galaxy in the field with respect to the cluster centre. Nis the total number of galaxies observed. and is the intrinsic logarithmic slope of the number counts. | the log-likelihood equation takes the form: where $n_0$ is the unlensed number density of background galaxies $^{-2}$ ), $\mu$ is the magnification, ${\mathbf \theta}_{i}$ is the position vector of the $i$ th galaxy in the field with respect to the cluster centre, $N$ is the total number of galaxies observed, and is the intrinsic logarithmic slope of the number counts. |
Vhe first term in the log-likelihood function addresses the probability. of finding Α΄ galaxies in the field of view given the lens model (6) and the | The first term in the log-likelihood function addresses the probability of finding $N$ galaxies in the field of view given the lens model $\mu(\theta)$ and the |
cameras were turned off. | cameras were turned off. |
During αμ]λίαν to mid-August 1997. the satellite was in a standby mode. with roth cameras turned on but without sufficient stabilization for seusitive imagine. | During mid-May to mid-August 1997, the satellite was in a standby mode, with both cameras turned on but without sufficient stabilization for sensitive imaging. |
During 103.1 d on-source time with a net exposure time of 27.8 d. the secondary observations coverec the field around the supernova remnant Cas A. This exposure is roughly uniformly distributed iu time. | During 103.4 d on-source time with a net exposure time of 27.8 d, the secondary observations covered the field around the supernova remnant Cas A. This exposure is roughly uniformly distributed in time. |
The latest data that we report here were obtained on Dec. 15. 1999. | The latest data that we report here were obtained on Dec. 15, 1999. |
Except for Cas A. there are uo bright Nav ποον present iu this field. | Except for Cas A, there are no bright X-ray sources present in this field. |
Compared to the background levels in the WECs. Cas A is uot so bright. | Compared to the background levels in the WFCs, Cas A is not so bright. |
The sensitivity --s. therefore. close to optimuun in the field. | The sensitivity is, therefore, close to optimum in the field. |
During two oestances. a relatively faint transient turned up in the field. at an angular distance of frou Cas A. They were on March. 1. 1997. aud May. 8. 1999. | During two instances, a relatively faint transient turned up in the field, at an angular distance of from Cas A. They were on March 4, 1997, and May 8, 1999. |
We note that sometimes Ce X-2 is in he same field of view as this transicut. but at an augular distauce of wwhich nmuplies it does not degrace the signal of he transient. | We note that sometimes Cyg X-2 is in the same field of view as this transient, but at an angular distance of which implies it does not degrade the signal of the transient. |
The celestial position of the WFC-detected trausicut ds 2000.0=22H 39MIINY, ὄορυυυ = wwith a coufideuce error radius of 1788. | The celestial position of the WFC-detected transient is $\alpha_{\rm 2000.0}=~22^{\rm h}$ $^{\rm m}$ $^{\rm s}$, $\delta_{2000.0}$ = with a confidence error radius of 8. |
The detection in March. 1997. was the strongest WEC detection obtained so far. | The detection in March, 1997, was the strongest WFC detection obtained so far. |
In Fie. 1.. | In Fig. \ref{figwfclcop}, |
we present a ligh curve with a resolution of about a day. | we present a light curve with a resolution of about a day. |
The period over which we detected activity is about 1 week. | The period over which we detected activity is about 1 week. |
The variation in brightuess during this event seenis to sugeest that i was not active for much longer. | The variation in brightness during this event seems to suggest that it was not active for much longer. |
A light curve of the second WFEC-detected outburs ix presented in Fie. 2.. | A light curve of the second WFC-detected outburst is presented in Fig. \ref{figwfclcop2}. |
The measured peak fiux of this outburst is about a factor of 3 lower than hat of the firs outburst but this could very well be a sampling effect. | The measured peak flux of this outburst is about a factor of 3 lower than that of the first outburst but this could very well be a sampling effect. |
The source was above the detection threshold for one week bu due to an uufavorable sampling it could just as well have been active for 50 davs. | The source was above the detection threshold for one week but due to an unfavorable sampling it could just as well have been active for 50 days. |
We have extracted the spectiuu from the observation at the peak of the fist outbirst aud modeled it with a simple power law plus absorption due to interstellar σας of cosnuic abundances (according to Morrison MeCiinuiuo- 1983). | We have extracted the spectrum from the observation at the peak of the first outburst and modeled it with a simple power law plus absorption due to interstellar gas of cosmic abundances (according to Morrison McCammon 1983). |
We kept thevalue for the ivdrogen «οπι density Ny fixed at 1.0&1072 7, as found from HI maps (Dickey Lockinan 1990). | We kept thevalue for the hydrogen column density $N_{\rm H}$ fixed at $1.0\times10^{22}$ $^{-2}$, as found from HI maps (Dickey Lockman 1990). |
The fit was satisfactory. wit[um ο.=1.22 (26 dof). | The fit was satisfactory, with $\chi^2_{\rm r}=1.22$ (26 dof). |
The photon index is quite hard at Lit0.1. | The photon index is quite hard at $-1.1\pm0.1$ . |
The spectrum is shown in Fie. 3.. | The spectrum is shown in Fig. \ref{figwfcspectrum}. |
The 2-1 keV fiux is 3.3S10Mere wwhich is 0.016. times he flux of the Crab in the same bandpass. | The 2-10 keV flux is $3.3\times10^{-10}$ which is 0.016 times the flux of the Crab in the same bandpass. |
Iu he cnerey range 2 to 26 keV the flux is 1.0410? oor 0.033 times that of he Crab. | In the energy range 2 to 26 keV the flux is $1.0\times10^{-9}$ or 0.033 times that of the Crab. |
Iu Fie. l.. | In Fig. \ref{figwfclc}, |
we present a light curve with a relatively hnieh time resolution when the flux was at maxiuuu durius the first outburst. | we present a light curve with a relatively high time resolution when the flux was at maximum during the first outburst. |
The source appears to be variable but no coherent signal could be found iu this data set. | The source appears to be variable but no coherent signal could be found in this data set. |
The confidence upper limit on the amplitude of a periodic sinusoidal variation is for periods between Land 10? «s. We have analyzed WEC data taken on December 13- 1999. | The -confidence upper limit on the amplitude of a periodic sinusoidal variation is for periods between 1 and $^3$ s. We have analyzed WFC data taken on December 13-15, 1999. |
This is 2 weeks after the optical measurements described in Sect. 6.. | This is 2 weeks after the optical measurements described in Sect. \ref{secopt}. . |
No N-rav cletection wasfouud. | No X-ray detection wasfound. |
The upper limit on the N-vav dux is 61011 ((2-10 keV). | The upper limit on the X-ray flux is $\times10^{-11}$ (2-10 keV). |
done e.g. for Cepheids (Butler et al.. 1996)). | done e.g. for Cepheids (Butler et al., \cite{butler}) ). |
The spectra preseuted in this paper do not have the necessary to-noise aud plase coverage for such purpose. | The spectra presented in this paper do not have the necessary signal-to-noise and phase coverage for such purpose. |
A method for obtaining “snapshot” distauces to SNe Ia has been developed very receutly by Riess ot al. (1998)). | A method for obtaining “snapshot” distances to SNe Ia has been developed very recently by Riess et al. \cite{riess2}) ). |
The idea is the following: one can calculate the distance of the SN by comparing a single BV or BVRI photometric mcasurement with a calibrated template SN Ia elt curve (describing the absolute magnitude of an “ideal” SN Ta as a function of tino) if the phase of the photometric data and the "lieht-curve parameter A (giving the magnitude difference between the waxinuun brightucss of the observed and the template SN) is known. | The idea is the following: one can calculate the distance of the SN by comparing a single $BV$ or $BVRI$ photometric measurement with a calibrated template SN Ia light curve (describing the absolute magnitude of an “ideal” SN Ia as a function of time) if the phase of the photometric data and the “light-curve parameter” $\Delta$ (giving the magnitude difference between the maximum brightness of the observed and the template SN) is known. |
A template SN Ja elt curve has been eiveu by Riess et al. (1996). | A template SN Ia light curve has been given by Riess et al. \cite{riess}) ). |
For the determination of A. a correlation is found between A and the ratio of line depths of the Si IT absorption lines at 58OO and 6150 (Nugent et al.. 1995: | For the determination of $\Delta$, a correlation is found between $\Delta$ and the ratio of line depths of the Si II absorption lines at 5800 and 6150 (Nugent et al., \cite{nugent}; |
Riess ct al. L998) ). | Riess et al., \cite{riess2}) ). |
We tried to apply the inethod outlined above using the first spectrum. obtained on April 22th. | We tried to apply the method outlined above using the first spectrum, obtained on April 22th. |
As the first step. we normalized the spectrmu to the σοιμα by fitting a snmoothlv varving Chebvshev-fuuction to the highest flux levels of the spectrum in order to correct for the steep echue of the intensity toward longer wavelcneths. | As the first step, we normalized the spectrum to the continuum by fitting a smoothly varying Chebyshev-function to the highest flux levels of the spectrum in order to correct for the steep decline of the intensity toward longer wavelengths. |
After that. we measured the line depths of the Si II troughs as shown in Fie. | After that, we measured the line depths of the Si II troughs as shown in Fig. |
3.3.2c (following the prescription elven w Nugent ct al. 1995)). | \ref{fig_3} (following the prescription given by Nugent et al., \cite{nugent}) ). |
The ratio. R. of these depths were then caleulated. resulting im A(Si ID) = d(5800À))/d(6150A&)) = 0.22+0.02. | The ratio, $R$, of these depths were then calculated, resulting in $R$ (Si II) = $d$ $/d$ ) = $0.22 \pm 0.02$ . |
Using the linear relationship between R(Si ID and A at f=7 davs relative to manxinuun lel (Riess et ab. 1905). | Using the linear relationship between $R$ (Si II) and $\Delta$ at $t=-7$ days relative to maximum light (Riess et al., \cite{riess2}) ), |
A=0.06£0.03 was derived. | $\Delta = 0.06 \pm 0.03$ was derived. |
The low value of A means that the helt curve of SN 1998aqwey not deviate larecly from the teiiplate SN Ta light curve {mut it should. of course. be proven by extensive photometry of the SN. which. uufortunatelv. was uot available or us during the preparation of the manuscript). | The low value of $\Delta$ means that the light curve of SN 1998aq not deviate largely from the template SN Ia light curve (but it should, of course, be proven by extensive photometry of the SN, which, unfortunately, was not available for us during the preparation of the manuscript). |
Strictly speaking. the calibration of R(Si ID) esA uses the phase # (iu days) relative to the D.ineccimum of the SN lieht curve (Riess ot ab. 1998)). | Strictly speaking, the calibration of $R$ (Si II) $vs~\Delta$ uses the phase $t$ (in days) relative to the $B-maximum$ of the SN light curve (Riess et al., \cite{riess2}) ). |
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