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The list of fields with clevation above 207 was prepared bw startup scripts. | The list of fields with elevation above $\arcdeg$ was prepared by startup scripts. |
During normal execution of patrol. for each of those fields wo δ second exposures woulda be taken. separated only x the 1.5 iinute duty evcle. | During normal execution of a patrol, for each of those fields two 80 second exposures would be taken, separated only by the 1.5 minute duty cycle. |
Reduced exposure time of 20 seconds was used in bright Moon helt couditions (73054 of data). | Reduced exposure time of 20 seconds was used in bright Moon light conditions $\sim$ of data). |
No frames were taken when the moou was closer han 12° from the field center. | No frames were taken when the moon was closer than $\arcdeg$ from the field center. |
Time keeping accurate to 20 18 was implemented using Network Time Protocol. | Time keeping accurate to 20 ms was implemented using Network Time Protocol. |
Ou a good nieht. it was possible to cover the eutire local sky (10.000 dee?) twice. | On a good night, it was possible to cover the entire local sky $\sim 10,000$ $^2$ ) twice. |
Paired observations are useful for detecting variability aud aperiodic trausieuts. | Paired observations are useful for detecting variability and aperiodic transients. |
They also provide a handle ou spurious detections due to πιαμιας space objects; cosmic ravs. hot pixels aud other effects. | They also provide a handle on spurious detections due to man-made space objects, cosmic rays, hot pixels and other effects. |
The position angle of the cameras was fixed at PAZ in all fields except for uear-polar region where the control software allowed PA=180". | The position angle of the cameras was fixed at $\arcdeg$ in all fields except for near-polar region where the control software allowed $180\arcdeg$. |
Iu the latter case. fields normally assigned to camerasa audb would be inaged by calneras and respectively. | In the latter case, fields normally assigned to cameras and would be imaged by cameras and respectively. |
Such observations are flageed appropriately and excluded from parts of the analvsis (Section 3.2.3)). | Such observations are flagged appropriately and excluded from parts of the analysis (Section \ref{sec:compilation}) ). |
Analysis of the data presented in this release was conducted offline on archival ROTSE-I images. | Analysis of the data presented in this release was conducted off-line on archival ROTSE-I images. |
Tere we byietle discuss the data reduction pipeline. schematically shown in Figure l.. which was emiploved to analyze that data. | Here we briefly discuss the data reduction pipeline, schematically shown in Figure \ref{fig:pipeline}, which was employed to analyze that data. |
Between August 1997 and December 2001. ROTSE-I collected 7 TB of unaee data. however the performance of the system was not optimal in the first few mouths of the project and near the eud of its lifetime. | Between August 1997 and December 2001, ROTSE-I collected 7 TB of image data, however the performance of the system was not optimal in the first few months of the project and near the end of its lifetime. |
To build the NSVS. we selected observations covering 1 full vear between April 1999 aud Mirch 2000. when the svstei delivered the best overall data quality. | To build the NSVS, we selected observations covering 1 full year between April 1999 and March 2000, when the system delivered the best overall data quality. |
This limited the raw data set to 225.000 images (~2 TD). | This limited the raw data set to 225,000 images $\sim$ 2 TB). |
The system would automatically prepare a median dark frame for each exposure time using all dark muages collected ou a particular observing welt. | The system would automatically prepare a median dark frame for each exposure time using all dark images collected on a particular observing night. |
Dark subtraction removes a siuall fraction of pixels (<1%)) with high dark current rates. | Dark subtraction removes a small fraction of pixels $\ll$ ) with high dark current rates. |
Flat field frames were obtained from a iedian of all individual patrol inages made durius a given nieht. | Flat field frames were obtained from a median of all individual patrol images made during a given night. |
This is possible with a large uuuber of independent fields (80) aud statistics iuited by sky noise due to large pixel size. | This is possible with a large number of independent fields $\sim$ 80) and statistics limited by sky noise due to large pixel size. |
Stellar profiles are conipletely removed by the procedure. | Stellar profiles are completely removed by the procedure. |
We fouud that shutter problems (Section 2.2)) affected some of the flat Ποια mages. | We found that shutter problems (Section \ref{sec:cameras}) ) affected some of the flat field images. |
Therefore. we visually evaluated all flat field ioannes and their ratios with frames made on a few other üehlts to select calibration sets with consisteut large scale xoperties. | Therefore, we visually evaluated all flat field frames and their ratios with frames made on a few other nights to select calibration sets with consistent large scale properties. |
As a result. it was possible to correct the vast uajoritv of the frames using &ood calibration frames from he same might or the might before. | As a result, it was possible to correct the vast majority of the frames using good calibration frames from the same night or the night before. |
The corrected images are passed to SExtractor software (Bertin Arnouts 1996) which reduces them to object ists. | The corrected images are passed to SExtractor software (Bertin Arnouts 1996) which reduces them to object lists. |
The choice of this source extraction package was notivated bv the undersampliug of stellar profiles. the sienificant eradieuts of the PSF shape in very wide ficld mages. aud overall reduction speed. | The choice of this source extraction package was motivated by the undersampling of stellar profiles, the significant gradients of the PSF shape in very wide field images, and overall reduction speed. |
SExtractor was 6Xtinized for reduction of ages in galaxy surveys. but it is known to perform well in moderately crowded stellar fields. | SExtractor was optimized for reduction of images in galaxy surveys, but it is known to perform well in moderately crowded stellar fields. |
Iu order to optimize seusitivity. our nuages are Altered before. object detection with a Gaussian kernel cluploving a EWIIM of 2.5 pixels aud requiring a iii of 5 connected pixels in an object. | In order to optimize sensitivity, our images are filtered before object detection with a Gaussian kernel employing a FWHM of 2.5 pixels and requiring a minimum of 5 connected pixels in an object. |
These basic detections are further thresholded by the software aud an attempt is made to break up blended objects; | These basic detections are further thresholded by the software and an attempt is made to break up blended objects. |
We use SExtractor aperture maenitudes calculated with the 5 pixel (72) aperture diameter. | We use SExtractor aperture magnitudes calculated with the 5 pixel $\arcsec$ ) aperture diameter. |
Since the ROTSE-I images are aliuost completely dominated bw stars. we store only a small fraction of information available for cach object: position. magnitude. magnitude error aud processing flags. | Since the ROTSE-I images are almost completely dominated by stars, we store only a small fraction of information available for each object: position, magnitude, magnitude error and processing flags. |
The observed errors at the bright cud of the maguitude rauge are larecr than predicted by simple photon noise. | The observed errors at the bright end of the magnitude range are larger than predicted by simple photon noise. |
Such discrepancies are conumon for CCD icasuremcuts aud are typically ecnerated by residual svstematic effects of flat field errors. thin clouds. PSF variations aud. sampling. | Such discrepancies are common for CCD measurements and are typically generated by residual systematic effects of flat field errors, thin clouds, PSF variations and sampling. |
In order to account for these systematic errors. we had to add. iu quadrature. a 0.01 mae contribution to the formal error bars. | In order to account for these systematic errors, we had to add, in quadrature, a 0.01 mag contribution to the formal error bars. |
SExtractor does not perform PSF photometry. aud iu eoncral it is unable to debleud liebt distributions without a saddle poiut. | SExtractor does not perform PSF photometry, and in general it is unable to deblend light distributions without a saddle point. |
This sets the distance Πατ of about 3.0 pixels for separation of stellar blends. | This sets the distance limit of about 3.0 pixels for separation of stellar blends. |
We fouud that the default parameters of the debleuder were verv conservative. resulting iu very large patches of the sky at low Galactic latitudes beiug assigned to the same objects. | We found that the default parameters of the deblender were very conservative, resulting in very large patches of the sky at low Galactic latitudes being assigned to the same objects. |
After some experimentation we were able to partially control this process. however. there are still cases when tight eroups of several objects with mergiug wines are considered to be a single object. | After some experimentation we were able to partially control this process, however, there are still cases when tight groups of several objects with merging wings are considered to be a single object. |
Typically. such aggregates extend up to ten pixels across with a bright object iu | Typically, such aggregates extend up to ten pixels across with a bright object in |
type IT ACN as high redshift radio galaxies! (IzRCs. > 2) | type II AGN as 'high redshift radio galaxies' (HzRGs, $z>2$ ). |
However. recently racdio-quict type IT AGN at Dom2 have also been fouud iusubnuuimiainDodyCitationEund325|ivi98s. X- and optical survevs2002). | However, recently radio-quiet type II AGN at $z>2$ have also been found insubmm, X-ray and optical surveys. |
. Despite these new developments. radio galaxies remain amouest the best studied galaxies at Lighredshift. because hey represent some of the most luminous stellar svsteiis shown out to.>52002). | Despite these new developments, radio galaxies remain amongst the best studied galaxies at high redshift, because they represent some of the most luminous stellar systems known out to $z>5$. |
. For example. deep optical spectropolarimetry cau reveal a wealth of information ou he stellar population of the host galaxy1991).. the presence of a scattered quasar component2001a).. and the kinematics. iouizatiou nechanisin aud metallicity of the extended emissiou line regions2000b). | For example, deep optical spectropolarimetry can reveal a wealth of information on the stellar population of the host galaxy, the presence of a scattered quasar component, and the kinematics, ionization mechanism and metallicity of the extended emission line regions. |
. Their cunission lines (especially Lya)) are often right enough to derive information on the deusitv aud netallicity of associated absorbers2002). | Their emission lines (especially ) are often bright enough to derive information on the density and metallicity of associated absorbers. |
. The radio selection has the advantage of beiug iusensitive to the dust properties. unlike optical sclection techniques. which may muss heavily obscured xvsteuis. | The radio selection has the advantage of being insensitive to the dust properties, unlike optical selection techniques, which may miss heavily obscured systems. |
Such objects iav be identified bv them stroug dust cluission at far-IR waveleneths. | Such objects may be identified by their strong dust emission at far-IR wavelengths. |
Early observations at SOO pan and 1.2 nuni by aud detected strong thermal dust cinissiou iu the radio galaxies 1€ 11.17 (2= 3.8) and 8C 1125)635 (2= L25). suggesting that several Πέις do indeed contain significant amounts ofdust. | Early observations at 800 $\mu$ m and 1.2 mm by and detected strong thermal dust emission in the radio galaxies 4C 41.17 $z=3.8$ ) and 8C 1425+635 $z=4.25$ ), suggesting that several HzRGs do indeed contain significant amounts of dust. |
observed 19 1«:Ll radio galaxies at 850 jan using the SCUBA bolometer on the ΙΟΝΕΤ. | observed 47 $1<z<4.4$ radio galaxies at 850 $\mu$ m using the SCUBA bolometer on the JCMT. |
Even after correcting for the strong iegative k correction eects on the Ravleigh-Jeaus tai of the thermal dust spectu1993).. they found a substautial increase in the 850 san Ipuninosity with redshitt. | Even after correcting for the strong negative $k-$ correction effects on the Rayleigh-Jeans tail of the thermal dust spectrum, they found a substantial increase in the 850 $\mu$ m luminosity with redshift. |
This is coufirmed by(2003c).. who detect uore than half of the sources with SCUBA in a sunple of 15 radio galaxies at +>3. | This is confirmed by, who detect more than half of the sources with SCUBA in a sample of 15 radio galaxies at $z>3$. |
Such a redshitt dependence is not seen for quasars. whose nui aud subuiun luunmositv remains almost unchanged between ~2 and locd2003). | Such a redshift dependence is not seen for quasars, whose mm and submm luminosity remains almost unchanged between $z\sim 2$ and $z\sim 4$. |
. From a imatched sample of 1.37<22.0 quasars aud radio galaxies selected at 151 MITz. found that the quasars are actually =2 times brighter at subnun wavelengths than the radio galaxies. | From a matched sample of $1.37 < z < 2.0$ quasars and radio galaxies selected at 151 MHz, found that the quasars are actually $\simgt 2$ times brighter at submm wavelengths than the radio galaxies. |
They also find an anticcorrelation between the far-IR Iunuinositv aud radio size. and interpret this as a svuchronization between he jet-trigecringao event aud processes controlling the far-IR luminosity. | They also find an anti-correlation between the far-IR luminosity and radio size, and interpret this as a synchronization between the jet-triggering event and processes controlling the far-IR luminosity. |
A possible explanation for the difference vetween the (ub)uua redshift evolution of radio galaxies and quasars could then be that ITzZRCs are more massive. eadiug to a longer (sub)nmnrlhnuuninous phase due to a arecr supply of gas. | A possible explanation for the difference between the (sub)mm redshift evolution of radio galaxies and quasars could then be that HzRGs are more massive, leading to a longer (sub)mm-luminous phase due to a larger supply of gas. |
The relatively bright subuua fiux deusities of ITzRCis iuple that they contaiu dust masses of 10710? AL... assundue standard couversion factors (see 8L2). | The relatively bright submm flux densities of HzRGs imply that they contain dust masses of $10^8 - 10^9$ $_{\odot}$, assuming standard conversion factors (see 4.2). |
The presence of the ACN iutroduces an ambiguity on the mechanism powering this dust emission: direct heating by the AGN or heating by massive stars formed in starbursts2002)? | The presence of the AGN introduces an ambiguity on the mechanism powering this dust emission: direct heating by the AGN or heating by massive stars formed in starbursts? |
? Although the ACN could casily introduce suffiiieut enerev to produce this enission. an increasing uunber of authors have argued that the starbursts are the dominating mechanism2002). | Although the AGN could easily introduce sufficient energy to produce this emission, an increasing number of authors have argued that the starbursts are the dominating mechanism. |
. A strong argument in favour of the starburst origin is the detection of dust and CO emission from regions several teus of kpc away from the AGN2000). | A strong argument in favour of the starburst origin is the detection of dust and CO emission from regions several tens of kpc away from the AGN. |
. The high gas masses iuferred from he CO detections could then be the likely reservoirs ceding these massive starbursts. | The high gas masses inferred from the CO detections could then be the likely reservoirs feeding these massive starbursts. |
The presence of CO in such reservoirs muüplies that they must be (a least utiallv) ietal enriched. which is cousistent with the recent detection of lonized metal lines at scales of several cus of kpe in the +=2.922 radio ealaxy AIRC 2122003). | The presence of CO in such reservoirs implies that they must be (at least partially) metal enriched, which is consistent with the recent detection of ionized metal lines at scales of several tens of kpc in the $z=2.922$ radio galaxy MRC $-$ 242. |
. These metals may lave been deposited κ’ previous merecr events, or by ealaxy-scale outflows2002). | These metals may have been deposited by previous merger events, or by galaxy-scale outflows. |
. These lavee dust and molecular Sas WAasses are roenundiscen of the often huge hhaloes seen around WzRGs2003b). | These large dust and molecular gas masses are reminiscent of the often huge haloes seen around HzRGs. |
. Moreover. A baud observations show that IIZRCs are amonest the most massive galaxies kuown at cach redshift2002). | Moreover, $K-$ band observations show that HzRGs are amongst the most massive galaxies known at each redshift. |
. ITowever. to date. the relationship )etween the differeut eas aud dust componcuts and the AGN host ealaxv has remained elusive. | However, to date, the relationship between the different gas and dust components and the AGN host galaxy has remained elusive. |
What is the role in the galaxy formation process of the exteuded thalocs and the associated absorbers secu in the rest-rae UV emission lines? | What is the role in the galaxy formation process of the extended haloes and the associated absorbers seen in the rest-frame UV emission lines? |
Are they composed of primordial naterial. or have they been euriched by material frou the rost ealaxy’? | Are they composed of primordial material, or have they been enriched by material from the host galaxy? |
Are the dust aud CO reservoirs in any wav inked to these? | Are the dust and CO reservoirs in any way linked to these? |
Iu this paper. we report the discovery of dust and CO chussion in the +=3.087 radio galaxy D3 J2330|3927. | In this paper, we report the discovery of dust and CO emission in the $z=3.087$ radio galaxy B3 J2330+3927. |
This is only the third :>3 radio galaxy where CO has been detected. after LC 60.07 aud 6C 1908|72202000).. and despite several intensive searches1997b). | This is only the third $z>3$ radio galaxy where CO has been detected, after 4C 60.07 and 6C 1908+7220, and despite several intensive searches. |
. Moreover. the CO curission is coincident in velocity space with associated aabsorption iu the line. | Moreover, the CO emission is coincident in velocity space with associated absorption in the line. |
This shows for the first time that these different coluponents are indeed plysically related. and trace a massive reservolr surrounding the ACN host galaxy. | This shows for the first time that these different components are indeed physically related, and trace a massive reservoir surrounding the AGN host galaxy. |
Throughout this paper. we use a cosnologv with a A dominated Universe with Ty=65765 lau + |l ον=0.3 and O4= 0,7. | Throughout this paper, we use a cosmology with a $\Lambda-$ dominated Universe with $_0 = 65h_{65}$ km $^{-1}$ $^{-1}$, $\Omega_{\rm M}=0.3$ and $\Omega_{\Lambda}=0.7$ . |
At 2= 3.087. the Iuuinosity | At $z=3.087$ , the luminosity |
spanned by dlnu/dln without imposing restrictions on(dln theT/dln relativeP, signs of theP) gradients involved. | spanned by $(d\ln T/d\ln P, d\ln \mu/d\ln P)$ without imposing restrictions on the relative signs of the gradients involved. |
We can now frame our results, summarized in Figure 2,, in the context provided by observations and theoretical models addressing the temperature and structure of galaxy clusters. | We can now frame our results, summarized in Figure \ref{fig:f2}, in the context provided by observations and theoretical models addressing the temperature and composition structure of galaxy clusters. |
Figure 3 shows acomposition schematic of the temperature and mean molecular weightrepresentation profiles of a representative galaxy cluster. | Figure \ref{fig:f3} shows a schematic representation of the temperature and mean molecular weight profiles of a representative galaxy cluster. |
The profile sketched there resembles the results obtainedtemperature by observations (Vikhlininetal. whereas the mean molecular weight is akin 2006),,to helium sedimentation models (Bulbulprofileetal. 2011).. | The temperature profile sketched there resembles the results obtained by observations \citep{2006ApJ...640..691V}, whereas the mean molecular weight profile is akin to helium sedimentation models \citep{2011A&A...533A...6B}. |
If the peak in the takes place at a larger radius than the peak temperaturein the mean molecular then there are three distinct regions defined by the weight, of the temperature and composition | If the peak in the temperature takes place at a larger radius than the peak in the mean molecular weight, then there are three distinct regions defined by the signs of the temperature and composition gradients. |
These signs correspond to different quadrantsgradients. in the (dInT/d]nregionsP,dinu/d1nP) plane as shown in panel (d) in Figure 2.. | These regions correspond to different quadrants in the $(d\ln T/d\ln P, d\ln
\mu/d\ln P)$ plane as shown in panel (d) in Figure \ref{fig:f2}. |
The joint of Figures 1 and 2 allows us to understand the analysisimplications that mean molecular weight can have for the various regions of representative gradientscluster as in Figure 3.. | The joint analysis of Figures \ref{fig:f1} and \ref{fig:f2} allows us to understand the implications that mean molecular weight gradients can have for the various regions of a representative galaxy cluster as depicted in Figure \ref{fig:f3}. |
If the magnetica field in the galaxyinner ICM is depicted to the background temperature dT/dz>0, as perpendicularsuggested by the end states of initial gradientconfigurations with B= that are HBI-unstable but evolve to B=B,, then this regionB; is stable if du/dz=0 there could be overstable g-modes driven by radiative (although Balbus&Reynolds 2010)). | If the magnetic field in the inner ICM is perpendicular to the background temperature gradient $dT/dz>0$, as suggested by the end states of initial configurations with $B=B_z$ that are HBI-unstable but evolve to $B\approx B_x$, then this region is stable if $d\mu/dz = 0$ (although there could be overstable $g$ -modes driven by radiative cooling \citealt{2010ApJ...720L..97B}) ). |
However, if du/dz>0 this cooling is unstable to conduction modes. | However, if $d\mu/dz >0$ this region is unstable to conduction modes. |
If the field in the regionouter ICM is to the temperature magneticdT'/dz«0, as the parallelend states of initial gradient with B= that suggestedare byMTI-unstable but evolve to B= configurationsthen this regionD; is overstable to and unstable to B,,conduction modes even if dii/dz=0. | If the magnetic field in the outer ICM is parallel to the temperature gradient $dT/dz<0$, as suggested by the end states of initial configurations with $B=B_x$ that are MTI-unstable but evolve to $B\approx B_z$, then this region is overstable to $g$ -modes and unstable to conduction modes even if $d\mu/dz = 0$. |
A g-modesnegative in the mean molecular is unable to stabilize these gradientmodes and it can further drive weightunstable diffusion modes. | A negative gradient in the mean molecular weight is unable to stabilize these modes and it can further drive unstable diffusion modes. |
Therefore, even if the outer/inner ICM is stable to both the MTI and the HBI, it could be rendered unstable to modes driven by either conduction, or diffusion. | Therefore, even if the outer/inner ICM is stable to both the MTI and the HBI, it could be rendered unstable to modes driven by either gravity, conduction, or diffusion. |
Unless the field is gravity, to the background gradients, the magneticthat we have orthogonaldenoted as intermediate is to be regionunstable to conduction and diffusion modes, but not to likelygravity modes. | Unless the magnetic field is orthogonal to the background gradients, the region that we have denoted as intermediate is likely to be unstable to conduction and diffusion modes, but not to gravity modes. |
These g-modes, however, could be relevant if the temperature profile peaks at a smaller radius than the mean molecular weight profile. | These $g$ -modes, however, could be relevant if the temperature profile peaks at a smaller radius than the mean molecular weight profile. |
We will address the limit in which conduction is fast compared to the dynamical timescale in a forthcoming paper. | We will address the limit in which conduction is fast compared to the dynamical timescale in a forthcoming paper. |
This limit contains the generalization of the instabilities that become the MTI and the HBI in the limit of a homogeneous plasma. | This limit contains the generalization of the instabilities that become the MTI and the HBI in the limit of a homogeneous plasma. |
We thank Matthew Kunz, Aldo Serenelli, and Shantanu Mukherjee for useful discussions. | We thank Matthew Kunz, Aldo Serenelli, and Shantanu Mukherjee for useful discussions. |
MEP is to the Knud Hgjgaard Foundation for its grateful support. | MEP is grateful to the Knud jgaard Foundation for its generous support. |
SC acknowledges support from the Danishgenerous Research Council through FNU Grant No. | SC acknowledges support from the Danish Research Council through FNU Grant No. |
505100-50 - 30,168. | 505100-50 - 30,168. |
cach. such that when the three blocks are fixed together. as in Figure 3(b). the crystals make a hexagonal arragement. | each, such that when the three blocks are fixed together, as in Figure 3(b), the crystals make a hexagonal arragement. |
The crystal integrating cavities are coupled to the telescope by individual feed-horns. as shown in Figure 3(b). with a resolution of 14 aresec. as for the SCUBA sS50-jm array (Molland et abl. | The crystal integrating cavities are coupled to the telescope by individual feed-horns, as shown in Figure 3(b), with a resolution of 14 arcsec, as for the SCUBA $\mu$ m array (Holland et al., |
1999). | 1999). |
Phe “PIIUAIPER. focal plane. array can also be adjusted to mateh the SCUBA 450-j4m array if desired. although this mode was not used on this occasion. | The THUMPER focal plane array can also be adjusted to match the SCUBA $\mu$ m array if desired, although this mode was not used on this occasion. |
We chose not to make the feed-horns dilfraction-Iimited on the telescope because the dish surface accuracy is too Low to provide a significant fraction of the total incident. power in a dillraction-limited beam at this wavelength. | We chose not to make the feed-horns diffraction-limited on the telescope because the dish surface accuracy is too low to provide a significant fraction of the total incident power in a diffraction-limited beam at this wavelength. |
The focal plane array is mounted in a stand as shown in Figure 3(c) and the filter stack attached to the front of the arrav as seen in Ligure 3(d). | The focal plane array is mounted in a stand as shown in Figure 3(c) and the filter stack attached to the front of the array as seen in Figure 3(d). |
The whole array is cooled to iquicl Helium temperature (3.7 Ix at JOMT) in a lone hold-ime cervostat. built by Queen Mary. College. Instruments (now based at Carcdill University) anc Thomas. Keating Ltd. The svstem detector quantum eflicieney (12010) was measured in the laboratory. | The whole array is cooled to liquid Helium temperature (3.7 K at JCMT) in a long hold-time cryostat, built by Queen Mary College Instruments (now based at Cardiff University) and Thomas Keating Ltd. The system detector quantum efficiency (DQE) was measured in the laboratory. |
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