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Caleulations were performed owed. upon the optical set-up of the instrument at the elescope. including estimates of the dish surface accuracy. | Calculations were performed based upon the optical set-up of the instrument at the telescope, including estimates of the dish surface accuracy. |
Incorporating all of these factors we estimated before going to the telescope that the noise equivalent [lux density (NEED) of the JCAIT-THUAIPER. arrangement should be ~HOTO Jv (1σ1 Walker 2004). | Incorporating all of these factors we estimated before going to the telescope that the noise equivalent flux density (NEFD) of the JCMT-THUMPER arrangement should be $\sim$ 50–70 Jy $\sigma$ 1s – Walker 2004). |
The ervostat was mounted on the right Nasmivth platform of the JCMNUE. | The cryostat was mounted on the right Nasmyth platform of the JCMT. |
“Pwo lenses. made of high-density polvethvlene. were used. to bring the bean from. the telescope to the £/5.75. focus required. by FIIUMPELI, (Walker. ct al. | Two lenses, made of high-density polyethylene, were used to bring the beam from the telescope to the f/5.75 focus required by THUMPER (Walker et al. |
2003). | 2003). |
The instrument. was commissioned during Director's Discretionary Time in two 4-night observing runs on 2005 Alareh 20-23. and 2005 April 6-9. | The instrument was commissioned during Director's Discretionary Time in two 4-night observing runs on 2005 March 20-23, and 2005 April 6-9. |
Optical alignment ancl instrument sctup were carried out prior to this. | Optical alignment and instrument setup were carried out prior to this. |
Data acquisition was carried out. via à. stand-alone. computer operating the LabVIEW software svsteni (Laboratory Virtual Instrument. Engineering Workbench). | Data acquisition was carried out via a stand-alone computer operating the LabVIEW software system (Laboratory Virtual Instrument Engineering Workbench). |
Only one of the scheduled: nights was good. enough. for astronomical observations at this wavelength. 2005 April 9. when our observing was scheduled [rom 01.30. to 09.30. Llawaiian Standard Time (UT. 11.30 to 19.30). | Only one of the scheduled nights was good enough for astronomical observations at this wavelength, 2005 April 9, when our observing was scheduled from 01.30 to 09.30 Hawaiian Standard Time (UT 11.30 to 19.30). |
Data from that night are presented in this paper. | Data from that night are presented in this paper. |
(Mag | \citep{mag98}. |
orriauetal.1998). | \citep{fab95} \citep{mao98}. |
. (Fabian&Rees1995) (Maoz1O98).. Mg. M. Ale. AlpucdnsALL. Ale=2.2isAL.yyL (Fjan&Caniza‘esLOSS:Mahadevau1997). | $M_{\rm BH}$ $\dot{M}$ $\dot{M}_{\rm E}$ $M_{\rm BH} = 10^8 m_8~M_{\sun}$ $\dot{M}_{\rm E} =
2.2 m_8~M_{\sun}~{\rm yr}^{-1}$ \citep{fab88,mah97}. |
.Bondi(1952) T=10'Tz P=109P; cmEw rpL3&17 ~1.9x10ns;M.vrHL asx=1 2;=mn Tz=1 Mp~1L.9x1071AZ, LF. My=2.2M. | Magorriaetal.(1998) | \citet{bon52} $T = 10^7 T_7$ $P = 10^6
P_6$ $^{-3}$ $r_{\rm B} \sim 4.3 m_8 T_7$ $\dot{M}_{\rm
B} \sim 1.9\times10^{-4} m_8 P_6 T_7 ~M_{\sun}~{\rm yr}^{-1}$ $m_8 = 1$ $P_6 =1$ $T_7 = 1$ $\dot{M}_{\rm B} \sim
1.9\times10^{-4}~M_{\sun}$ $^{-1}$ $\dot{M}_{\rm E}
= 2.2~M_{\sun}$ $^{-1}$ \citet{mag98} \citet{nar98}. |
The most obvious environmental elfect appears to be the population of low surface brightness ciSphs discovered bv Alieskectal.(2007) in the Fornax cluster. | The most obvious environmental effect appears to be the population of low surface brightness dSphs discovered by \cite{mi07} in the Fornax cluster. |
Where an environmental influence is clearly ciscernible. it has only mild effects on the scaling relations. | Where an environmental influence is clearly discernible, it has only mild effects on the scaling relations. |
The presence of a low-surface brightness population of Fornax dSphs doesn't allect he global scaling relation appreciably. | The presence of a low-surface brightness population of Fornax dSphs doesn't affect the global scaling relation appreciably. |
At a given Luminosity. he Fornax dSph population is on average 0.2 mag aresec7 zünter than the Perseus and Local Group dsph populations. | At a given luminosity, the Fornax dSph population is on average 0.2 mag $^{-2}$ fainter than the Perseus and Local Group dSph populations. |
The M1. companions with tidal extensions or distorsions (Scéealletal.2007:Lewis20€Ἡ are not displaced from he general scaling relations. | The M31 companions with tidal extensions or distorsions \citep{s07,l07} are not displaced from the general scaling relations. |
“This may indicate that cSphs intrinsically have high. enough Al/L to survive unscathed (sce Pennyetal. (2008))) or that dSphs with too low ML aave been destroved and only those with hieh M/L survive o the present clay. | This may indicate that dSphs intrinsically have high enough M/L to survive unscathed (see \cite{pe08}) ) or that dSphs with too low M/L have been destroyed and only those with high M/L survive to the present day. |
SDR. wishes to thank Philippe Prugnicl ancl Mina. Ixoleva for their hospitality and for the stimulating discussions while visiting CRAL Lyon Observatory curing the course of this work. | SDR wishes to thank Philippe Prugniel and Mina Koleva for their hospitality and for the stimulating discussions while visiting CRAL Lyon Observatory during the course of this work. |
CJC and SJP acknowledge: support. [rom STEC. | CJC and SJP acknowledge support from STFC. |
SDR is a tlow of the Fund. for Scientific Research - Flanders. Poon"Ke(Belgium)(E..O). | SDR is a Postdoctoral Fellow of the Fund for Scientific Research - Flanders (Belgium)(F.W.O). |
SV. is a PhD Fellow of the Fund Scientific Research - FlandersNASA(Belgium)(E.N.O). | SV is a PhD Fellow of the Fund for Scientific Research - Flanders (Belgium)(F.W.O). |
Ες research has mace use of the IPAC Extragalactic Database (NED) which is operated. by the Jet Propulsion Laboratory. California Institute of Technology. under contract with the National Acronautics and Space Administration. | This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. |
colors). small ealactocentric radii. and the lareer-(han-average sizes. a portion may also be the stripped nuclei of dwarl galaxiesanalogues of w Cen in the Galaxy (Majewski 2000). | colors), small galactocentric radii, and the larger-than-average sizes, a portion may also be the stripped nuclei of dwarf galaxies—analogues of $\omega$ Cen in the Galaxy (Majewski 2000). |
The color distribution of cE nuclei in (his sample (see below) peaks al g—z1.01.1. consistent wilh the blue end of the intermecdiate-color objects. | The color distribution of dE nuclei in this sample (see below) peaks at $g-z \sim 1.0-1.1$, consistent with the blue end of the intermediate-color objects. |
The surface brightness profiles ol these objects resemble those of other GCs and do not have the exponential proliles seen in some ullra-compact dwarf galaxies (de Propris 2005). (hough we note our size selection criterion [or GCs would exclude some Virgo UCDs (IIasegan 2005). | The surface brightness profiles of these objects resemble those of other GCs and do not have the exponential profiles seen in some ultra-compact dwarf galaxies (de Propris 2005), though we note our size selection criterion for GCs would exclude some Virgo UCDs (Hasegan 2005). |
Similar bright. intermeciate-color GC's have also been found in the NGC 1399 (Dirsch 2003). NGC 4636 (Dirsch. Schuberth. Riehtler 2005). and NGC 1407 (Cenarro 2005): they appear to be a common feature of οἱ». | Similar bright, intermediate-color GCs have also been found in the NGC 1399 (Dirsch 2003), NGC 4636 (Dirsch, Schuberth, Richtler 2005), and NGC 1407 (Cenarro 2005); they appear to be a common feature of gEs. |
A feature present in the CMDs of M&7 and NGC 4649 is a of the color distribution of blue GCs. in the sense that the mean color of the blue GCs becomes recder with increasing Iuminositv. | A feature present in the CMDs of M87 and NGC 4649 is a of the color distribution of blue GCs, in the sense that the mean color of the blue GCs becomes redder with increasing luminosity. |
No such trend is apparent for the red GCs. | No such trend is apparent for the red GCs. |
A precise measure of this observation is challenging: due to the multiple subpopulations aud "II GC's. a direct linear fit is nol viable. | A precise measure of this observation is challenging; due to the multiple subpopulations and “H” GCs, a direct linear fit is not viable. |
Instead. we divided the AIST GC candidates into four 0.5 mag bins in the range 20<2<22 and one 0.4 mag bin (22.8<223.2. avoiding the "II GCs). | Instead, we divided the M87 GC candidates into four 0.5 mag bins in the range $20 < z < 22$ and one 0.4 mag bin $22.8 < z < 23.2$, avoiding the “H" GCs). |
To each of these bins we fit a heteroscedastic normal mixture model. aud then fit à weighted linear model to the resulting blue peaks. | To each of these bins we fit a heteroscedastic normal mixture model, and then fit a weighted linear model to the resulting blue peaks. |
This model is g—2=—0.043z+1.848: the slope is to signilicant. | This model is $g-z = -0.043 \, z + 1.848$; the slope is $4 \sigma$ significant. |
A fit to the corresponding red peaks is consistent wilh a slope of zero. | A fit to the corresponding red peaks is consistent with a slope of zero. |
These fits. as well as the binned values. are overplotted on the M87 CMD in Figure 2. | These fits, as well as the binned values, are overplotted on the M87 CMD in Figure 2. |
Including a bin with the "II GCs (22<2« 22.8) gives a slope which is (uisurprisinglv) slightly more shallow (—0.037) but still significant. | Including a bin with the “H” GCs $22 < z <
22.8$ ) gives a slope which is (unsurprisingly) slightly more shallow $-0.037$ ) but still significant. |
NGC 4649 has fewer GC's (han M87 and appears to have no Ἡ GCs, so for this galaxy we fit three 1.0 mag bins in the range 20<2«23. | NGC 4649 has fewer GCs than M87 and appears to have no “H” GCs, so for this galaxy we fit three 1.0 mag bins in the range $20 < z < 23$. |
The resulting blue GC modelis g—2=—0.040z+L.817. which agrees verv well with that of M87. and there is again no significant evidence for a nonzero red GC slope. | The resulting blue GC model is $g-z = -0.040
\, z + 1.817$, which agrees very well with that of M87, and there is again no significant evidence for a nonzero red GC slope. |
The smoothuess of the change argues against stochastic stellar population changes (e.g.. horizontal branch stars. blue stragglers) as the cause of the trend. | The smoothness of the change argues against stochastic stellar population changes (e.g., horizontal branch stars, blue stragglers) as the cause of the trend. |
If due to age. ils ~0.12— mag in g—2 over ~2 mag in 2) would require an unlikely age spread of ~7—8 Gvr ab low metallicity using Maraston (2005) models. | If due to age, its $\sim 0.12-0.13$ mag in $g-z$ over $\sim 3$ mag in $z$ —would require an unlikely age spread of $\sim 7-8$ Gyr at low metallicity using Maraston (2005) models. |
If due to metallicity. the colormetallicity relation derived above indicates the trend corresponds (ο a mean slope of ~0.15—0.2 dex/mag. | If due to metallicity, the color–metallicity relation derived above indicates the trend corresponds to a mean slope of $\sim 0.15-0.2$ dex/mag. |
For blue GC's in these galaxies.mass. | For blue GCs in these galaxies,. |
Interpretations of (his surprising finding are discussed below: first we consider whether a bias in observation or analvsis might be the cause. | Interpretations of this surprising finding are discussed below; first we consider whether a bias in observation or analysis might be the cause. |
peaks located at lower energies and are more ganaray dominated than their fainter (and eeuerally lower redshitt) analogues. | peaks located at lower energies and are more gamma–ray dominated than their fainter (and generally lower redshift) analogues. |
Within the blazar population. high-redshift objects are the most luninous aud generally belong to the class of Flat-Spectrum Radio Quasars (FSRQ). | Within the blazar population, high-redshift objects are the most luminous and generally belong to the class of Flat-Spectrum Radio Quasars (FSRQ). |
Observations of hiegh-huninosity blazars in the Xοrav baud are particularly important (expecially if available over a broad energy range} as they allow the characterization of the inverse Compton peak aud related parameters. | Observations of high-luminosity blazars in the X–/gamma–ray band are particularly important (especially if available over a broad energy range) as they allow the characterization of the inverse Compton peak and related parameters. |
More specifically. a fattening in the spectral distribution of the seed photons producing Xravs via inverse Compton is often observed at low energies iu the Xraw spectra of these objects and cau be measured only with broad band data (see e.g. Tavecchio et al. | More specifically, a flattening in the spectral distribution of the seed photons producing X–rays via inverse Compton is often observed at low energies in the X–ray spectra of these objects and can be measured only with broad band data (see e.g. Tavecchio et al. |
2007 aud references therein). | 2007 and references therein). |
Uufortunatebv. the situation is far more couples. as absorption iutrinsic to the source can also reproduce the spectral curvature observed iu the X.ray baud (e.g.. Page et al | Unfortunately, the situation is far more complex, as absorption intrinsic to the source can also reproduce the spectral curvature observed in the X–ray band (e.g., Page et al. |
2005: Yuan et al. | 2005; Yuan et al. |
2006): in this case. information ou the absorption is useful to understaud the source environnient and its relation to the jet. | 2006); in this case, information on the absorption is useful to understand the source environment and its relation to the jet. |
Besides this. X/feanuuaray observations can provide evidence for the existence of extreme blazirs. ie. those with the svuchrotron peak Iwing at Nταν energies (Cao et al. | Besides this, X–/gamma–ray observations can provide evidence for the existence of extreme blazars, i.e. those with the synchrotron peak lying at X–ray energies (Giommi et al. |
2007: Bassani et al. | 2007; Bassani et al. |
2007). | 2007). |
ere. we report detailed information on a new. powerful and hard Xray. seleeted blazar. Swift 23302. receutlv discoverec through hieh- observations made with Swift/BAT aud INTECRAL/IBIS. | Here, we report detailed information on a new, powerful and hard X–ray selected blazar, Swift $-$ 3302, recently discovered through high-energy observations made with /BAT and /IBIS. |
We preseut the results of our optical follow-up work. which has allowed the identification of the source with a blazar at redshift 7 = 2.1. along with an accurate analvsis of the available Suvftf/XRT aud INTECRAL/IDIS data. | We present the results of our optical follow-up work, which has allowed the identification of the source with a blazar at redshift $z$ = 2.4, along with an accurate analysis of the available /XRT and /IBIS data. |
We also construct a SED for Swift 3302 and discuss the characteristics of the source road band emission. | We also construct a SED for Swift $-$ 3302 and discuss the characteristics of the source broad band emission. |
The paper is structured as follows: Sect. | The paper is structured as follows: Sect. |
2 reports a collection of the main results available iu the literature ou this source: Sects. | 2 reports a collection of the main results available in the literature on this source; Sects. |
3 and { illustrate the optical aud hieh-eneorgv observations. respectively: Sect. | 3 and 4 illustrate the optical and high-energy observations, respectively; Sect. |
5 contains the results of this observational campaign. while a discussion ou them is elven iu Sect. | 5 contains the results of this observational campaign, while a discussion on them is given in Sect. |
6. | 6. |
Conclusions are outlined in Sect. | Conclusions are outlined in Sect. |
T. | 7. |
Throughout the paper. aud uuless otherwise specified. uncertainfies are given at the confidence level. | Throughout the paper, and unless otherwise specified, uncertainties are given at the confidence level. |
We also assuue a cosnologv with fy = το au ! +. OQ, = 0,7 and O,, = 0.3. | We also assume a cosmology with $H_0$ = 70 km $^{-1}$ $^{-1}$ , $\Omega_\Lambda$ = 0.7 and $\Omega_{\rm m}$ = 0.3. |
The ligh-cucrey source Swift 3302 was discovered with the BAT imager (Darthehuw ct al. | The high-energy source Swift $-$ 3302 was discovered with the BAT imager (Barthelmy et al. |
2005) onboard theSwift satellite (Gehrels et al. | 2005) onboard the satellite (Gehrels et al. |
2001) diving a survey performed between December 2001 aud September 2005 (Okajima et al. | 2004) during a survey performed between December 2004 and September 2005 (Okajima et al. |
2006). | 2006). |
The object was detected at coordinates RA = 16 56" 192. Dec = 33° 01 ts” (J2000). which are about 673 from the Galactic Plane. aud with a positional uncertaiuty of 12% | The object was detected at coordinates RA = $^{\rm h}$ $^{\rm m}$ $\fs$ 2, Dec = $-$ $^\circ$ $'$ $''$ (J2000), which are about $\fdeg$ 3 from the Galactic Plane, and with a positional uncertainty of $'$. |
Okajima et al. ( | Okajima et al. ( |
2006) also reported that the Ll200 keV BAT spectrum was very hard with a photon iudex DP-1.340.5. alc with+ a fux ofm 1.0410. 29 exe D7? ο, | 2006) also reported that the 14–200 keV BAT spectrum was very hard with a photon index $\Gamma$ $\pm$ 0.3, and with a flux of $\times$ $^{-10}$ erg $^{-2}$ $^{-1}$. |
TheY somce flux was variable by a factor of as high as 1. | The source flux was variable by a factor of as high as 4. |
Subsequent poiuted observations (Tueller et al. | Subsequent pointed observations (Tueller et al. |
2006) with Susft/NRT (Burrows ct al. | 2006) with /XRT (Burrows et al. |
2005) performed iu June 2006 located the Xrav counterpart at a position RA = 16 56" 1656. Dec= — 33? 02' 0973 σου). with au uncertainty of 377. | 2005) performed in June 2006 located the X–ray counterpart at a position RA = $^{\rm h}$ $^{\rm m}$ $\fs$ 56, Dec= $-$ $^\circ$ $'$ $\farcs$ 3 (J2000), with an uncertainty of $\farcs$ 7. |
The NRT data were fitted with an absorbed power law with P=1.l40.3 and Nyp = (3.94017) « 1023 2. | The XRT data were fitted with an absorbed power law with $\Gamma$ $\pm$ 0.3 and $_{\rm H}$ = $\pm$ $\times$ $^{21}$ $^{-2}$. |
By comparing this value with the Galactic absorption column density along the direction of Swift 3302 4107! 7: Dickey Lockanan 1990). Tueller et al. ( | By comparing this value with the Galactic absorption column density along the direction of Swift $-$ 3302 $\times$ $^{21}$ $^{-2}$; Dickey Lockman 1990), Tueller et al. ( |
2006) sueeestedOO that if may be an extragalactic object. | 2006) suggested that it may be an extragalactic object. |
These authors also measured au absorbed flux iu the 0.310 keV. band of 5.610. 12 ere 7? 3 aud predicted a flux in the LL195 keV baud of «10 More 2 1, comparable with the DAT detection of Okajima et al. ( | These authors also measured an absorbed flux in the 0.3–10 keV band of $\times$ $^{-12}$ erg $^{-2}$ $^{-1}$ and predicted a flux in the 14–195 keV band of $\times$ $^{-11}$ erg $^{-2}$ $^{-1}$, comparable with the BAT detection of Okajima et al. ( |
2006). | 2006). |
Tuecler ct al. ( | Tueller et al. ( |
2006) detected no sources with Swift/UVOT (Bomiug et al. | 2006) detected no sources with /UVOT (Roming et al. |
2005) in the NRT eror circle at a limiting maecuitude of 20 iu the ultraviolet flters. | 2005) in the XRT error circle at a limiting magnitude of 20 in the ultraviolet filters. |
The soft Xrav position of Swift 3302 is consisteut with theradio source NVSS 330211 (having a 1.1 CGIIz fiux density of LO0.7412.3 wiv: Condon et al. | The soft X–ray position of Swift $-$ 3302 is consistent with the radio source NVSS $-$ 330211 (having a 1.4 GHz flux density of $\pm$ 12.3 mJy; Condon et al. |
1998) and (albeit mareinally) with the faintROSAT source LRNS 2330150 (Voges et al. | 1998) and (albeit marginally) with the faint source 1RXS $-$ 330150 (Voges et al. |
2000). | 2000). |
According to Tueller et al. ( | According to Tueller et al. ( |
2006) theROSAT data indicate that. if the two sources are the same. spectral variability max be present. | 2006) the data indicate that, if the two sources are the same, spectral variability may be present. |
A second. weak X.rav source was also found with NRT within the BAT error circle. but Tueller et al. ( | A second, weak X–ray source was also found with XRT within the BAT error circle, but Tueller et al. ( |
2006) judged it too soft and faint to be the soft Nrav counterpart of the BAT source. | 2006) judged it too soft and faint to be the soft X–ray counterpart of the BAT source. |
Swift 3302 was also fouud to be associated with an unidentified source in the 373 IDIS survey of Bird et al. ( | Swift $-$ 3302 was also found to be associated with an unidentified source in the $^{\rm rd}$ IBIS survey of Bird et al. ( |
2007). with average 260LO keV and 10100 keV fluxes of 9.1410. 12 ore 7s 1 aud 1.1410. H ere 28 4 respectively, assunüng a Crab-ike spectrum. | 2007), with average 20–40 keV and 40–100 keV fluxes of $\times$ $^{-12}$ erg $^{-2}$ $^{-1}$ and $\times$ $^{-11}$ erg $^{-2}$ $^{-1}$, respectively, assuming a Crab-like spectrum. |
According to these observations. the source ies at coordinates RA = 169 569 901, Ώου 33° pr 4972 (J2000). | According to these observations, the source lies at coordinates RA = $^{\rm h}$ $^{\rm m}$ $\fs$ 4, Dec= $-$ $^\circ$ $'$ $\farcs$ 2 (J2000). |
The error circle is 2/5 in radius. | The error circle is $\farcm$ 5 in radius. |
This osition is cousisteut with the BAT and NRT positions reported above. | This position is consistent with the BAT and XRT positions reported above. |
Iu the following. we further analyze this source over a xoad range of frequencies. | In the following, we further analyze this source over a broad range of frequencies. |
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