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Figure 7 shows the 2uuu PdBI data. integrated between 112.515 CIIz and 112.723 GIIz. which represeuts the full width of the redshifted CO 7=13 line (see below). | Figure \ref{COoverlay} shows the 3mm PdBI data, integrated between 112.515 GHz and 112.723 GHz, which represents the full width of the redshifted CO $J=4-3$ line (see below). |
The cluission clearly peaks at the position of objecte. which is the most likely position of the AGN (see 3.2). | The emission clearly peaks at the position of object, which is the most likely position of the AGN (see 3.2). |
The enission docs uot follow the extension of the radio source. confirming that a possible sxuchrotrou contribution would be minimal. | The emission does not follow the extension of the radio source, confirming that a possible synchrotron contribution would be minimal. |
Figure 8. shows the PdBI CO 7=Ll3 spectu of D3 J2330|3927 extracted at the position of objecta. | Figure \ref{B3COposa} shows the PdBI CO $J=4-3$ spectrum of B3 J2330+3927 extracted at the position of object. |
We show the uubiuned spectrum. aud a spectrum binned to 105|. | We show the unbinned spectrum, and a spectrum binned to 105. |
A broad cussion liue is clearly seeu around 112.6 CGIIz. with a weak uuderblvius contiuuun eniüssion. | A broad emission line is clearly seen around 112.6 GHz, with a weak underlying continuum emission. |
We fit a Gaussian profile with an underline continui chussion to determine the line aud continu parameters. | We fit a Gaussian profile with an underlying continuum emission to determine the line and continuum parameters. |
Table lL eives the fit parameters for 5 different biu sizes used. | Table \ref{3mmfit} gives the fit parameters for 5 different bin sizes used. |
As lone as the biu size does not exceed LO MIITz. the derived parameters are not very sensitive to the biu widths. | As long as the bin size does not exceed 40 MHz, the derived parameters are not very sensitive to the bin widths. |
Iu the xevious section. we estimated the coutrbution from svuchrotron euission to be «0.5 mJy. so the broad. ~2 indy liue appears securely detected. | In the previous section, we estimated the contribution from synchrotron emission to be $<0.5$ mJy, so the broad, $\sim$ 2 mJy line appears securely detected. |
We iuterpret this enmission liue as CO F=lo3 at Ξ001. ooffset by ~500 tto the red from the optical redshift. determined from the line. | We interpret this emission line as CO $J=4-3$ at $z=3.094$, offset by $\sim$ 500 to the red from the optical redshift, determined from the line. |
Such offsets have also been seen in high S/N CO identifications of high redshift quasars2 | Such offsets have also been seen in high S/N CO identifications of high redshift quasars. |
002a).. The ~0.3 indy contin emission seen in the 1.3 nun spectrum (Fie. 8)) | The $\sim$ 0.3 mJy continuum emission seen in the 1.3 mm spectrum (Fig. \ref{B3COposa}) ) |
is consistent with the extrapolation of the thermal dust spectitun (Fie. 6)). | is consistent with the extrapolation of the thermal dust spectrum (Fig. \ref{B3SED}) ), |
but it is also likely that there is a svuchrotron contribution from the northern radio | but it is also likely that there is a synchrotron contribution from the northern radio |
Johnston Melrose (1995). Ball et al. ( | Johnston Melrose (1995), Ball et al. ( |
1999) and. Connors et al. ( | 1999) and Connors et al. ( |
2002). | 2002). |
Unpulsed emission has also been detected in the X-ray (summarised in Hiravama et al. | \nocite{jml+96,jmmc99,cjmm02,mjm95,bmjs99}
Unpulsed emission has also been detected in the X-ray (summarised in Hirayama et al. |
1996) and in the soft οταν band. by Crove et al. ( | 1996) and in the soft $\gamma$ -ray band by Grove et al. ( |
1995) and. more recently Shaw et al. ( | 1995) and more recently Shaw et al. ( |
2004). with modelling of the emission described in Tavani Arons (1997). | 2004), with modelling of the emission described in Tavani Arons (1997). |
νι]. Ball ancl Skjaeraasen proposed that the system should be detectable at high energies through inverse Compton scattering of the UV. photons from the Be star by the relativistic pulsar wind. | \nocite{hnt+96,gtp+95,ta97,scr+04}
Kirk, Ball and Skjaeraasen \nocite{kbs99} proposed that the system should be detectable at high energies through inverse Compton scattering of the UV photons from the Be star by the relativistic pulsar wind. |
TFhis model has largely. been confirmed through a recent detection of the svstem at ‘TeV energies by Aharonian ct al. (2004). | This model has largely been confirmed through a recent detection of the system at TeV energies by Aharonian et al. \nocite{aaa+04}. |
. Observations of the pulsar were carried out with the 64-nm radio telescope located in Parkes. NSW. at frequencies between 680 and SO40. Alli. | Observations of the pulsar were carried out with the 64-m radio telescope located in Parkes, NSW, at frequencies between 680 and 8640 MHz. |
Two independent backend systems. were emploved: filterbank systems which recorded. total power ari a correlator system which retained full polarisation information. | Two independent backend systems were employed; filterbank systems which recorded total power and a correlator system which retained full polarisation information. |
The filterbank system was used. at GSO ane 1500 Mllz only. | The filterbank system was used at 680 and 1500 MHz only. |
At the lower frequency it consists of 256 requency channels cach of width: 0.250 MlIIZz lor a tota ranclwidth of G4 MlIz and at the higher frequency consists of 512 frequency. channels cach of width 0.5 MlIz for a tota xinciwidth of 256 MlIz. | At the lower frequency it consists of 256 frequency channels each of width 0.250 MHz for a total bandwidth of 64 MHz and at the higher frequency consists of 512 frequency channels each of width 0.5 MHz for a total bandwidth of 256 MHz. |
In cach case the analogue signal is one-hit digitised every 250 yes and written to tape for oll-line analysis. | In each case the analogue signal is one-bit digitised every 250 $\mu$ s and written to tape for off-line analysis. |
This analysis involved de-clispersion and folding a he topocentric period to produce a pulse profile. | This analysis involved de-dispersion and folding at the topocentric period to produce a pulse profile. |
Correlator data were obtained at. frequencies around. 1370. 3100. ac S640 MlIIZz with a total bandwidth of 256. 512 and 512 MllIz al 1e three frequencies. | Correlator data were obtained at frequencies around 1370, 3100 and 8640 MHz with a total bandwidth of 256, 512 and 512 MHz at the three frequencies. |
Channel banedwidths were 1. MIIz and there were 512 phase bins across the pulsar period. | Channel bandwidths were 1 MHz and there were 512 phase bins across the pulsar period. |
The data were folded on-line for an interval of GO s and written to disk. | The data were folded on-line for an interval of 60 s and written to disk. |
Oll-line. processing used. the software application (?) specifically written for analvsis of pulsar data. | Off-line processing used the software application \cite{hvm04} specifically written for analysis of pulsar data. |
Processing involved calibration and de-dispersion and vielded Pull Stokes pulse profiles. | Processing involved calibration and de-dispersion and yielded full Stokes pulse profiles. |
In a typical observation. data were obtained. at 680. 1500. 3100 and N640 MlIz in the space of 3 h. The time- CEA) of the fiducial point in the pulsar. profile was calculated. for each observation. by convolving with a standard. template which is frequcney dependent. | In a typical observation, data were obtained at 680, 1500, 3100 and 8640 MHz in the space of 3 h. The time-of-arrival (ToA) of the fiducial point in the pulsar profile was calculated for each observation by convolving with a standard template which is frequency dependent. |
The emplates at different frequencies were aligned in pulse phase as shown in Ligure 1 of Wang et al. ( | The templates at different frequencies were aligned in pulse phase as shown in Figure 1 of Wang et al. ( |
2004). | 2004). |
Any olfset )etween the arrival times at the dillerent frequencies. was hen attributed to a change in dispersion measure (DM) of he pulsar and a fit was done to obtain the ollset DAL. | Any offset between the arrival times at the different frequencies was then attributed to a change in dispersion measure (DM) of the pulsar and a fit was done to obtain the offset DM. |
The polarisation information allowec us to obtain the rotation measure (RAL) for cach observation. | The polarisation information allowed us to obtain the rotation measure (RM) for each observation. |
There are wo possible methods for obtaining the RAL | There are two possible methods for obtaining the RM. |
The first. is o measure the change in position angle across the band. | The first is to measure the change in position angle across the band. |
This can be done either at a given pulsar phase or by time averaging across several phase bins. | This can be done either at a given pulsar phase or by time averaging across several phase bins. |
The second method is to maximise the linearly. polarised Iux by choosing trial ItMs. | The second method is to maximise the linearly polarised flux by choosing trial RMs. |
This method. works well for low signal to noise ratios as it uses the entire pulse window. | This method works well for low signal to noise ratios as it uses the entire pulse window. |
In fact. for63.. there is very. little change in the position angle across cach component. and the two methods vield similar results. | In fact, for, there is very little change in the position angle across each component, and the two methods yield similar results. |
Table 1. shows the log of the observations of the pulsar mace with the Parkes telescope. | Table \ref{dmrm} shows the log of the observations of the pulsar made with the Parkes telescope. |
The first column gives the date of the observation and. the second. column shows the olfset. in days from the 2004. periastron epoch (which we denote as hhereafter). | The first column gives the date of the observation and the second column shows the offset in days from the 2004 periastron epoch (which we denote as hereafter). |
Observations were also made with the Australia Telescope Compact Array (ATCA). an cast-west synthesis telescope located: near Narrabri. NSW. which consists of six 22-m antennas on a 6 km track. | Observations were also made with the Australia Telescope Compact Array (ATCA), an east-west synthesis telescope located near Narrabri, NSW, which consists of six 22-m antennas on a 6 km track. |
ATCA observations can be mace simultaneously at either 14 and 2.4 Giz or 4.8 and 8.4 612 with a bandwidth of 128 Mllz at cach frequeney subdivided into 32 spectral channels. and. full Stokes parameters. | ATCA observations can be made simultaneously at either 1.4 and 2.4 GHz or 4.8 and 8.4 GHz with a bandwidth of 128 MHz at each frequency subdivided into 32 spectral channels, and full Stokes parameters. |
The ATCA is also capable of splitting cach correlator evcele into bins corresponding to different phases of a pulsar's period. and in our case the pulse period. of ~48 ms was split into 16 phase bins. | The ATCA is also capable of splitting each correlator cycle into bins corresponding to different phases of a pulsar's period, and in our case the pulse period of $\sim$ 48 ms was split into 16 phase bins. |
This allows a measurement of oll-pulse and on-pulse [ux densities to be made simultaneously. | This allows a measurement of off-pulse and on-pulse flux densities to be made simultaneously. |
Initial data reduction and analysis were carried out with the package using standard. techniques. | Initial data reduction and analysis were carried out with the package using standard techniques. |
After ageing bac data. the primary calibrator was used. for | After flagging bad data, the primary calibrator was used for |
We now consider the other verv metal-poor clusters in our sample: M92. MIS. and NGC 5053. | We now consider the other very metal-poor clusters in our sample: M92, M15, and NGC 5053. |
studied carbon ancl nitrogen abundances in M92 from the SGB to the AGB. and reported a general decrease in C abundances moving to higher huninosiües. but no correlation or anticorrelation between the C and N abundances. | studied carbon and nitrogen abundances in M92 from the SGB to the AGB, and reported a general decrease in C abundances moving to higher luminosities, but no correlation or anticorrelation between the C and N abundances. |
Instead. they determined (hat the total number of C-+N atoms varies from star lo star within (he cluster. an observation at odds with predictions that the sum ought to remain constant. | Instead, they determined that the total number of C+N atoms varies from star to star within the cluster, an observation at odds with predictions that the sum ought to remain constant. |
Similar conclusions were reached by regarding δις C abundance drops as one moves up the RGB. but N abundance remains on average (he same. although with some uncorrelated star-to-star variations. | Similar conclusions were reached by regarding M15 – C abundance drops as one moves up the RGB, but N abundance remains on average the same, although with some uncorrelated star-to-star variations. |
A more recent study of MIS by also failed to detect reliable evidence of CN bimodality. although thev confirmed (he existence of a verv small number of CN-enriched stars. also reported by (1992). | A more recent study of M15 by also failed to detect reliable evidence of CN bimodality, although they confirmed the existence of a very small number of CN-enriched stars, also reported by . |
. A recent study by of NGC 5466 ~—2.2) suggested the possible presence of two CN groups. with a small mean separation of only 0.055. | A recent study by of NGC 5466 $\simeq -2.2$ ) suggested the possible presence of two CN groups, with a small mean separation of only 0.055. |
Thev noted that the generalized histogram of their RGB stars was not well-deseribecl by a single Gaussian fit. | They noted that the generalized histogram of their RGB stars was not well-described by a single Gaussian fit. |
In a similar fashion. we examined the generalized histograms for RGB stars in the verv metal-poor clusters M92. M15. and NGC 5053. | In a similar fashion, we examined the generalized histograms for RGB stars in the very metal-poor clusters M92, M15, and NGC 5053. |
Figure 8. shows the histogranms for these clusters. as well as that of NGC 5466 Irom(2010).. fit with a single Gaussian: residuals are plotted in the insets in each panel. | Figure \ref{figm92m15n5053n5466rgbgenhist}
shows the histograms for these clusters, as well as that of NGC 5466 from, fit with a single Gaussian; residuals are plotted in the insets in each panel. |
The residuals [rom the fits to our three very metal-poor clusters are clearly larger than (hose of NGC 5466. suggesting that our data also max not be well-described by a single Gaussian population. | The residuals from the fits to our three very metal-poor clusters are clearly larger than those of NGC 5466, suggesting that our data also may not be well-described by a single Gaussian population. |
ILowever. a IXMM test for each cluster (including NGC 5466) cannot reject the null hvpothesis that a single population well-describes the observed data. indicating that hints of the non-Gaussian distributions in our data may simply be due to small-i» statistics. | However, a KMM test for each cluster (including NGC 5466) cannot reject the null hypothesis that a single population well-describes the observed data, indicating that hints of the non-Gaussian distributions in our data may simply be due to $n$ statistics. |
If these clusters possess multiple CN behaviors. thev may not be discernible within (he present measurement uncertainties. | If these clusters possess multiple CN behaviors, they may not be discernible within the present measurement uncertainties. |
Due to the fact that double-metal molecules like CN are particularly. difficult | Due to the fact that double-metal molecules like CN are particularly difficult |
The ratio of total transverse to total lougittdinal (observer frame) momentum 2/2! in the shell is the same as the ratio egtBOLU eiven [rom equations (18)) and (19)). which is iudependent of position. | The ratio of total transverse to total longitudinal (observer frame) momentum $P_R/P'_z$ in the shell is the same as the ratio $\bar v_R/\bar v_z'=\beta c_s/v_s$ given from equations \ref{eq:meanvelz}) ) and \ref{eq:meanvelR}) ), which is independent of position. |
Since this ratio is less tlan oue. the shell will have more forward- than sideways-directed motion. althougihead the transverse motion exceeds lougitudinal motion (since mining is ve‘y incomplete iu the shell). | Since this ratio is less than one, the shell will have more forward-directed than sideways-directed motion, although the transverse motion exceeds longitudinal motion (since mixing is very incomplete in the shell). |
Because the "bulk" aud spatially-resolvecl kinematics of jet-driven slells are so clifferent. it is crucial to obtain observations in order to make cdiscerimilating comparisons with theoretical mioclels. | Because the “bulk” and spatially-resolved kinematics of jet-driven shells are so different, it is crucial to obtain high-resolution observations in order to make discriminating comparisons with theoretical models. |
Ii tliis paper. we have constructed au aualytic dynamical model for the shape and kinematics of the vow shock shell created. when a protostellar jet tunpacts the surrounding (undisturbed) interste uiedium. | In this paper, we have constructed an analytic dynamical model for the shape and kinematics of the bow shock shell created when a protostellar jet impacts the surrounding (undisturbed) interstellar medium. |
Morphologically. the shell consists of two parts: the “working surface." a jockey-puck-shaped region of radius 2; where the jet collides cirectly with the ambient meciu and surrouudiug “wings” at 2>A; which separate the low-density “cocoon” of shocked jet ο rou. uidisturbed ambient mecium (see Fie. | Morphologically, the shell consists of two parts: the “working surface,” a hockey-puck-shaped region of radius $\sim R_j$ where the jet collides directly with the ambient medium, and surrounding “wings” at $R>R_j$ which separate the low-density “cocoon” of shocked jet gas from the undisturbed ambient medium (see Fig. |
1). | 1). |
The shell is composed of ambient. materi swept V yw the acvatcing bow shock. with deusities aud. pressures high iu worki rlace a ower | le wines. | The shell is composed of ambient material swept up by the advancing bow shock, with densities and pressures high in working surface and lower in the wings. |
We analyze the flow iu the wines in detail: the workiug surfac eion is. our 1uodel. analyzed soely to estimate the mass aud momeutum flow it ejects into tl rouncli necdiui | We analyze the flow in the wings in detail; the working surface region is, in our model, analyzed solely to estimate the mass and momentum flow it ejects into the surrounding medium. |
ΤΙe chief siniplifviug assuimptio1 we invoke in our auavsls is that thermal pressure forces play aniiportant role ouly in the working surface at the head o ‘the jet. but not iu the wines of the bow shocς, | The chief simplifying assumption we invoke in our analysis is that thermal pressure forces play an important role only in the working surface at the head of the jet, but not in the wings of the bow shock. |
Au initial transverse monentui imipulse (perpeudictar to the jet. and locally taugential to he slell’s surface) and mass input are applied to the shell flow i ithe wings at 4?—Rj. | An initial transverse momentum impulse (perpendicular to the jet, and locally tangential to the shell's surface) and mass input are applied to the shell flow in the wings at $R=R_j$. |
Subsequent o this impulse. the shell flow expands away [rorn the axis and sweeps up ambient material in a lisο [ashion — Le. conserviug the total mass aud momenta of tle shell + swept-up ambient . | Subsequent to this impulse, the shell flow expands away from the axis and sweeps up ambient material in a ballistic fashion – i.e. conserving the total mass and momenta of the shell + swept-up ambient material. |
Physically. it is the radial pressure gracieus within tle Workine surface that impar “ALISVe‘se impulse to the shell in the wines. | Physically, it is the radial pressure gradients within the working surface that impart the initial transverse impulse to the shell in the wings. |
The iitial mass flux to the wings is provi : ambient eas which has entered the working surace th‘ough its οuter face. then been racla “ECirected auc expelled from the sides of the workiue surace. | The initial mass flux to the wings is provided by ambient gas which has entered the working surface through its outer face, then been radially redirected and expelled from the sides of the working surface. |
The ballistic shell’s shape a1 1 velocities iu tle wines depeud ou the ambient densiy. the shock speec TM and ou the initial valuesilt of uass audd momentum flows emerging perpeucicularly from the working surface (but not o a detaiec itlenal dyuaimiics). | The ballistic shell's shape and the velocities in the wings depend on the ambient density, the shock speed $v_s$, and on the initial values of mass and momentum flows emerging perpendicularly from the working surface (but not on its detailed internal dynamics). |
Becase he shocked. ambient gas in the wo‘kine surface cools5 rapidly to ~ 104. with COLTespolkling sound speed c;Skinsl the 4ransverse velocity vjC, ol the gas input to the shell £‘on the working surface will be small compared to its longitulial (observer reference frame) velocily ve.vy along the jet axis. | Because the shocked ambient gas in the working surface cools rapidly to $\sim 10^4$ K, with corresponding sound speed $c_s\sim 8\kms$, the transverse velocity $v_R\sim c_s$ of the gas input to the shell from the working surface will be small compared to its longitudinal (observer reference frame) velocity $v_z=v_s$ along the jet axis. |
Memory of this ratio is preserved as the mean ratio Φου Owith © an order-unity constant) of transverse/longitudital momenta in the wings of the sliell (see Fig. | Memory of this ratio is preserved as the mean ratio $\beta c_s /v_s$ (with $\beta$ an order-unity constant) of transverse/longitudinal momenta in the wings of the shell (see Fig. |
(2aa)). | \ref{fig:shape}a a)). |
This strongly forward-directecd mean tlirust is respousible for the high degree | This strongly forward-directed mean thrust is responsible for the high degree |
This paper took great advantage from discussions with Anna Gallazzi and Jarle Brinchmann, who kindly provided us with all the details of their stellar masses calculations using DR4 and DR7, respectively. | This paper took great advantage from discussions with Anna Gallazzi and Jarle Brinchmann, who kindly provided us with all the details of their stellar masses calculations using DR4 and DR7, respectively. |
Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for The SDSS Web Site is:http://www.sdss.org/.. | Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for The SDSS Web Site is:. |
We are grateful to the anonymous referee, whose comments and remarks helped us to improve the quality and the readability of this work. | We are grateful to the anonymous referee, whose comments and remarks helped us to improve the quality and the readability of this work. |
shakes similar to. or perhaps more effective than. (hose torquegenerated by impacts. | shakes similar to, or perhaps more effective than, those generated by impacts. |
Consequently. surface morphologv may be modilied. ( | Consequently, surface morphology may be modified. ( |
2) The tidal nav spin up an asteroid. | 3) The tidal torque may spin up an asteroid. |
In surface segments where the centrifugal force exceedsMore gravity. regolith“changes layers will be removed bycarrving away the excess angular momentum. | In surface segments where the centrifugal force exceeds gravity, regolith layers will be removed by carrying away the excess angular momentum. |
subtle can occur in other surface parts of a spun-up asteroid. ( | More subtle changes can occur in other surface parts of a spun-up asteroid. ( |
4) If the tidal Loree becomes comparable to the objects eravily curing encounter. an asteroid with large enough internal strength ancl a strengthless regolith max lose its regolith laver. | 4) If the tidal force becomes comparable to the object's gravity during encounter, an asteroid with large enough internal strength and a strengthless regolith may lose its regolith layer. |
These effects and their dependence on the encounter distance and speed are poorly understood. | These effects and their dependence on the encounter distance and speed are poorly understood. |
Some insights into (his problem can be obtained [rom Richardson et al. ( | Some insights into this problem can be obtained from Richardson et al. ( |
1993). where the authors performed numerical simulations of the effects of tidal gravity on a small asteroid with strengthless (rubble-pile) interior. | 1998), where the authors performed numerical simulations of the effects of tidal gravity on a small asteroid with strengthless (rubble-pile) interior. |
In the most favorable case (slow encounter speed. [ast prograde rotation). (hey found that significant mass shedding can occur up to 2:5 fiy. | In the most favorable case (slow encounter speed, fast prograde rotation), they found that significant mass shedding can occur up to $\approx$ 5 $R_{\rm pl}$. |
This sets à soft constraint on (cá. | This sets a soft constraint on $r^*$. |
On one hand. 7 can be larger than 5 Ay because the opticallv-active (hin surface laver may be vulnerable (o even tiniest perturbations that were not considered in the Richardson et al. | On one hand, $r^*$ can be larger than 5 $R_{\rm pl}$ because the optically-active thin surface layer may be vulnerable to even tiniest perturbations that were not considered in the Richardson et al. |
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