ReadingTimeMachine/rtm-sgt-ocr-v1 · Datasets at Hugging Face

source stringlengths 1 2.05k ⌀	target stringlengths 1 11.7k
This is interesting iu view of a determination of the total cnerey fiux along the jet (e.g. Celotti et al.	This is interesting in view of a determination of the total energy flux along the jet (e.g. Celotti et al.
1997. Sikora ct al.	1997, Sikora et al.
1997).	1997).
The total kinetic” power of the jet can be written as: where AR is the jet radius. D ds the bulk Lorentz factor aud Ü is the total energy deusitv in the jet. including radiation. magnetic field. relativistic particles aud eventually protous.	The total " kinetic" power of the jet can be written as: where $R$ is the jet radius, $\Gamma$ is the bulk Lorentz factor and $U$ is the total energy density in the jet, including radiation, magnetic field, relativistic particles and eventually protons.
If one assumes that there is 1 (cold) proton per relativistic electron. the proton contribution is usually dominant.	If one assumes that there is 1 (cold) proton per relativistic electron, the proton contribution is usually dominant.
Iu Fig.	In Fig.
2 the derived radiative huninosity £44 aud kinetic power of the jet Pia for a group of sources with sufficieutlv good spectral information are compared.	2 the derived radiative luminosity $L_{\rm jet}$ and kinetic power of the jet $P_{\rm jet}$ for a group of sources with sufficiently good spectral information are compared.
The ratio between these two quantities eives directly the "radiative efficiency? of the jet. which turis out to be jj20.1. though with large scatter.	The ratio between these two quantities gives directly the “radiative efficiency” of the jet, which turns out to be $\eta\simeq 0.1$, though with large scatter.
The line traces the result of a least-squares ft: we found a slope ~1.3. suggesting a decrease ofthe radiative efficiency. with decreasing power.	The line traces the result of a least-squares fit: we found a slope $\sim 1.3$, suggesting a decrease of the radiative efficiency with decreasing power.
Two iain classes of models for the production of jets has been proposed.	Two main classes of models for the production of jets has been proposed.
The frst class considers the extraction of rotational enerev from the black	The first class considers the extraction of rotational energy from the black
dashed lines uutil they eventually intersect the cooling inflow at some large radius r,..	dashed lines until they eventually intersect the cooling inflow at some large radius $r_c$.
audThe europe of the bubbles and flow are identical atr, the bubbles provide Bonjust chough gas to maintain the inflowing cooling flow that radius.	The entropy of the bubbles and flow are identical at $r_c$ and the bubbles provide just enough gas to maintain the inflowing cooling flow from that radius.
The third row of paucls(ο. aud. À) shows the uegative cooling inflow with solid lines aud he much faster outward motion of the riiug bubbles. ej>.0. with dashed lines.	The third row of panels, and ) shows the negative cooling inflow with solid lines and the much faster outward motion of the rising bubbles, $u_b > 0$, with dashed lines.
The variation of the bubble radius ois shown in thebottom row of panels(df aud 2 with dash- lines.	The variation of the bubble radius $r_b(r)$ is shown in the bottom row of panels, and ) with dash-dotted lines.
The dashed lines iu these bottom panels show the variation of the inflow volume filling factor f(r).	The dashed lines in these bottom panels show the variation of the inflow volume filling factor $f(r)$.
As h approaches the highest possible value for each bubble mass mp. ho» huyus thebubbles nearly fill the eutire available volume at kj where f0 0. as explained by Condition (21).	As $h$ approaches the highest possible value for each bubble mass $m_b$, $h \rightarrow h_{max}$ , the bubbles nearly fill the entire available volume at $r_h$ where $f \rightarrow 0$ , as explained by Condition (21).
For the most massive bubbles cousidered. ay,=LO A... solutions for two heating parameters are shown. )—3 and 6 for which the circulation radi are r,LO and 25 kpe respectively.	For the most massive bubbles considered, $m_b = 10^6$ $M_{\odot}$, solutions for two heating parameters are shown, $h = 3$ and 6 for which the circulation radii are $r_c = 10$ and 25 kpc respectively.
The deusity. temperature and velocity profiles for the cooling inflows for these two solutions are alinost ideutical.	The density, temperature and velocity profiles for the cooling inflows for these two solutions are almost identical.
We have not considered larger values of h because thebubble velocity «, for the f=6 solution the sound speed iu the cooling flow (50/3)?=ee(T/lO Klaus. \|.	We have not considered larger values of $h$ because the bubble velocity $u_b$ for the $h = 6$ solution approaches the sound speed in the cooling flow $(5 \theta /3)^{1/2} = 476~(T/10^7~{\rm K})$ km $^{-1}$.
Larger / would result in supersonic bubble velocities that would drive shocks iuto the cooling eas. drsinatficallv increasing its temperature.	Larger $h$ would result in supersonic bubble velocities that would drive shocks into the cooling gas, dramatically increasing its temperature.
Also the bubble size attorj for the f=6 solution. η)~1 kpc Is Colmparable rp. again arene agaist larger values of h.	Also the bubble size at $r_h$ for the $h = 6$ solution, $r_b(r_h) \sim 1$ kpc is comparable to $r_h$, again arguing against larger values of $h$.
The ceutral column of Fiewe 2 illustrates two circulation flows forbubbles of mass me=Q0 AL. for h —3aud 6.5.	The central column of Figure 2 illustrates two circulation flows for bubbles of mass $m_b = 10^5$ $M_{\odot}$ for $h = 3$ and 6.5.
The circulation with —x6.5 extends out to =[8 kpc. but the flow fillime factor f less than abou Ll atory so there are uo circulations with fo6.5zchi, (Condition 21).	The circulation with $h = 6.5$ extends out to $r_c = 18$ kpc, but the flow filling factor $f$ is less than about 0.1at $r_h$ so there are no circulations with $h > 6.5 \approx h_{max}$ (Condition 21).
Iu order for this mareial flow to suppor unss flux M. the relative flow muo nuust as SOory, and the drag increases accordinely.	In order for this marginal flow to support mass flux ${\dot M}$ , the relative flow $u_b - u$ must increase as $r \rightarrow r_h$ and the drag increases accordingly.
The pirebubble velocity a, is secu to decline toward +).	The bubble velocity $u_b$ is seen to decline toward $r_h$.
As a result he laree drag. the effective eravity g,. (Equation 15) is directed outward near ry,lL kpe where the flow woul Ravleigh-Tavlor unstable.	As a result of the large drag, the effective gravity $g_e$ (Equation 15) is directed outward near $r_h = 1$ kpc where the flow would be Rayleigh-Taylor unstable.
This region of instability vecolmcs larger for higher values of 5.	This region of instability becomes larger for higher values of $h$.
Because of the approximations we have made. the deusitv in the flow region ry«or<r, is somewhat higher than the density observed iu NCC I172 (dotted lines).	Because of the approximations we have made, the density in the flow region $r_h < r < r_c$ is somewhat higher than the density observed in NGC 4472 (dotted lines).
However. if this flow were observed. the appareut density iyap, would be owered since the flow only occupies a fraction. f£ of the volume. Le. n,app!)29f2r).	However, if this flow were observed, the apparent density $n_{e,app}$ would be lowered since the flow only occupies a fraction $f$ of the volume, i.e., $n_{e,app}(r) \approx f^{1/2} n_e(r)$.
The frst cohuun in Fieure 2 shows the circulation ραίσα for bubbles of mass ney«10! AL. for two flows with h=3 aud	The first column in Figure 2 shows the circulation pattern for bubbles of mass $m_b = 3 \times 10^4$ $M_{\odot}$ for two flows with $h = 3$ and 3.6.
The flow fllius factor f is dropping rapidly as ro>ry for the f=3.6 solution so lis is close to the maximum possible heating (and 7.) for hese smallerbubbles.	The flow filling factor $f$ is dropping rapidly as $r \rightarrow r_h$ for the $h = 3.6$ solution so this is close to the maximum possible heating (and $r_c$ ) for these smaller bubbles.
We were unable to achieve fully convergent flow solutions with even sinallerbubbles of nass nn,S&SLO’ ALL.	We were unable to achieve fully convergent flow solutions with even smaller bubbles of mass $m_b \lta 10^4$ $M_{\odot}$ .
While our search for such solutions was not exhaustive. if is apparent from the trend im pauclsk »g > ein Figure 2 that the maximaun values of u;. 7 and r,. all decrease with my. as expected frou condition 22),	While our search for such solutions was not exhaustive, it is apparent from the trend in panels $\rightarrow$ $\rightarrow$ in Figure 2 that the maximum values of $u_b$, $h$ and $r_c$ all decrease with $m_b$, as expected from condition (22).
Bubbles of mass ai,=3<104 AL. are approaching the minima 25 necessary to carry the cooling mass flow AT foy auy heating 5h21.	Bubbles of mass $m_b = 3 \times 10^4$ $M_{\odot}$ are approaching the minimum $m_b$ necessary to carry the cooling mass flow ${\dot M}$ for any heating $h > 1$.
Nou-circulating flows with bubbles of lower mass must ultimately cool radiativelv to temperatures mich lower than Trj). iu disagreement with NADAL observations.	Non-circulating flows with bubbles of lower mass must ultimately cool radiatively to temperatures much lower than $T(r_h)$, in disagreement with XMM observations.
One of the motivations for our exploration of nou-rocks circulation flows is to estimate the influence of the bubbles on the apparent eas temperature which typically has a nuninuun near the origin.	One of the motivations for our exploration of non-cooling circulation flows is to estimate the influence of the bubbles on the apparent gas temperature which typically has a minimum near the origin.
To simulate the apparcut temperature that would be inferred when viewiug the cooling inflow aud the hot rising bubbles aloug the same lue of sight. we calculated the local cuission-weighted telpcrature which is plotted as dotted lines for each of the flows in panels5.f audj of Figure 2.	To simulate the apparent temperature that would be inferred when viewing the cooling inflow and the hot rising bubbles along the same line of sight, we calculated the local emission-weighted temperature which is plotted as dotted lines for each of the flows in panels, and of Figure 2.
For most circulation flows (7) is nearly iudistinguisliable frou the temperature of the cooling flow component.	For most circulation flows $\langle T\rangle$ is nearly indistinguishable from the temperature of the cooling flow component.
Consequcuth. a sinele phase interpretation of the temperature profile would show a mildly positive eradieut. dffdro>0. similar to those observed aud consisteut with traditional cooling flows.	Consequently, a single phase interpretation of the temperature profile would show a mildly positive gradient, $dT/dr > 0$, similar to those observed and consistent with traditional cooling flows.
This is a desirable feature of the circulation model.	This is a desirable feature of the circulation model.
Qu for the least iuassive bubbles cousidered. mdifferential«10! AL... does (P3 vise slightly as r>ry. but the change in the temperature profile caused by the hot bubbles is xnall.	Only for the least massive bubbles considered, $m_b = 3 \times 10^4$ $M_{\odot}$, does $\langle T\rangle$ rise slightly as $r \rightarrow r_h$, but the differential change in the temperature profile caused by the hot bubbles is small.
Tle apparent density pap)(C023)72. and eutropy profiles are also similar to those of the cooling flow component alouc.	The apparent density $\rho_{app} = (\langle \rho^2 \rangle)^{1/2}$ and entropy profiles are also similar to those of the cooling flow component alone.
We stress that these results differ from normal couvection where (1) there is a single temperature and density at every radius (apart from fluctuations). (2) the temperature eradieut is determined by the gravitational potential. dffdr=(270,ΕΙ fdr). aud theretore has a sig opposite to that observed. aud (3) the entropy is constant.	We stress that these results differ from normal convection where (1) there is a single temperature and density at every radius (apart from fluctuations), (2) the temperature gradient is determined by the gravitational potential, $dT/dr = -(2 \mu m_p/5 k)(d \Phi /dr)$ , and therefore has a sign opposite to that observed, and (3) the entropy is constant.
The ratio of Pd/V heating to drag heating is where a,«\|e] appropriateand sve use qzzLAF«10Ln cms ? whichis for lXors 1003 NCC 1172.	The ratio of $PdV$ heating to drag heating is where $u_b \ll \|u\|$ and we use $g \approx 4.47 \times 10^{-7} r_{kpc}^{-0.85}$ cm $^{-2}$ which is appropriate for $1 \lta r_{kpc} \lta 100$ in NGC 4472.
The result Z,4;/2,471 follows nunediately frou Equation (13) provided dui, ΠΜ	The result ${\dot \varepsilon}_{pdv}/{\dot \varepsilon}_d \sim 1$ follows immediately from Equation (13) provided $u_b \ll \|u\|$.
of the uncertain physical nature of these two comparablebubble-flow heating mechanisimnis. we cousider heating due to bubble expansion and drag separately,	In view of the uncertain physical nature of these two comparable bubble-flow heating mechanisms, we consider heating due to bubble expansion and drag separately.
Figure 23 illustrates four represcutative cooling flow models in which the work done by the drag force is assuned to leat the local cooling flow eas with various efficiencies ο) (aud Cyd.= 0).	Figure 3 illustrates four representative cooling flow models in which the work done by the drag force is assumed to heat the local cooling flow gas with various efficiencies $e_d$ (and $e_{pdv} = 0$ ).
As before AT07 M. t and ry,=1d kpe for allflows.	As before ${\dot M} = 0.7$ $M_{\odot}$ $^{-1}$ and $r_h = 1$ kpc for allflows.
The fourflows also have the same bubble mass a,=10° M. and heating factor 5h=6. but thebubble drag heating cfiicieucy has values e,= 0. 0.1. 0.3 and0.7.	The fourflows also have the same bubble mass $m_b = 10^5$ $M_{\odot}$ and heating factor $h = 6$, but the bubble drag heating efficiency has values $e_d = 0$ , 0.1, 0.3 and0.7.
Flows with progressively lugher T. 75 aud » near the heating radius ky correspoud to increasing efficiencies.	Flows with progressively higher $T$, $T_b$ and $n$ near the heating radius $r_h$ correspond to increasing efficiencies.
By contrast. the circulation radii. velocitics.filling factors audbubble radii are inscusitive to the heating efficieucy.	By contrast, the circulation radii, velocities,filling factors and bubble radii are insensitive to the heating efficiency.
However. the flow with the largest heating efiicieucy. ο=OF is less satisfactory because flow teniperature aud particularly the appareut temperature(75 develop appreciable negative radial gradieuts ucar rj.	However, the flow with the largest heating efficiency, $e_d = 0.7$ is less satisfactory because flow temperature and particularly the apparent temperature$\langle T \rangle$ develop appreciable negative radial gradients near $r_h$ .
Because of	Because of
seven of them show neeligible absorption. or do not show any band or line so they. were discarded for the gas mixtures.	Seven of them show negligible absorption, or do not show any band or line so they were discarded for the gas mixtures.
We have chosen high puritv gases commercially. available with deeper absorptions and wider spectral coverage. adding and/or replacing individual eases with new ones. includiug acetvlene. nitrous oxide. hydrocarbons ancl chloromethans. using different partial pressures.	We have chosen high purity gases commercially available with deeper absorptions and wider spectral coverage, adding and/or replacing individual gases with new ones, including acetylene, nitrous oxide, hydrocarbons and chloromethans, using different partial pressures.
All of them are safe (ο use at this small concentrations. are nol corrosive and are gaseous al room temperature: (his makes (hem suitable for regular eround-based In total we have worked with five new different. mixtures (see Figure 5)).	All of them are safe to use at this small concentrations, are not corrosive and are gaseous at room temperature; this makes them suitable for regular ground-based In total we have worked with five new different mixtures (see Figure \ref{fig2}) ).
We have listed the composition in Table 4..	We have listed the composition in Table \ref{tab2}.
Due to the number of gas cells available. only three have been measured twice for stability. study.	Due to the number of gas cells available, only three have been measured twice for stability study.
The first two new mixtures (namely Mixture-I. 111. included nitrous oxide. acetvlene. methane and/or ehloromethans: only Mixture-I was measured on (wo occasions three months apart.	The first two new mixtures (namely Mixture-I, II), included nitrous oxide, acetylene, methane and/or chloromethans; only Mixture-I was measured on two occasions three months apart.
We found Mixture-I to be stable. with differences on the measurements lower than on band absorption intensity and nnm on line position.	We found Mixture-I to be stable, with differences on the measurements lower than on band absorption intensity and nm on line position.
Dased on (his mixture. three additional mixtures introducing ammonia and hydrocarbons were produced. namely NIL;i-I. HH: and HII.	Based on this mixture, three additional mixtures introducing ammonia and hydrocarbons were produced, namely $_{3}$ -I, II and III.
The mixture δα Π was measured eight months apart and remained stable with time ancl temperature. but we have discarded methane because of the atmospheric absorption.	The mixture $_{3}$ -II was measured eight months apart and remained stable with time and temperature, but we have discarded methane because of the atmospheric absorption.
We have carried ont a characterization of the NIL4-HI gas cell bv means of an Infrared Fourier Transform (FTIR) Spectrometer (Domen DAS). located at the University of Central Florida (USA).	We have carried out a characterization of the $_{3}$ -III gas cell by means of an Infrared Fourier Transform (FTIR) Spectrometer (Bomen DA8), located at the University of Central Florida (USA).
The instrument makes use of a InSb (€ Indium Antimonice) detector. a cquartz-halogen lamp as source and a quartz beam-splitter.	The instrument makes use of a InSb ( Indium Antimonide) detector, a quartz-halogen lamp as source and a quartz beam-splitter.
The spectrum was obtained wider vacuum (< 5mTorr) at 23°C with a resolution of 0.1 + (R = 40000 at 2.5 jm).	The spectrum was obtained under vacuum $<$ 5mTorr) at $\degr$ C with a resolution of 0.1 $^{-1}$ (R = 40000 at 2.5 $\mu$ m).
The cell was measured with Cary 5 and on two separate occasions wilh FTIR. three and eight months apart.	The cell was measured with Cary 5 and on two separate occasions with FTIR three and eight months apart.
Figure ?? compares a high resolution measurement with the low resolution measurement. an ammonia gas cell NIL, + Argon). a M9 brown dwar moclel (I. ~ 65000) and a telluric spectra in absorption (from top to bottom).	Figure \ref{3} compares a high resolution measurement with the low resolution measurement, an ammonia gas cell $_{3}$ + Argon), a M9 brown dwarf model (R $\sim 65000$ ) and a telluric spectra in absorption (from top to bottom).
This gas cell consists on a mixture of NoO. Πο, CICIL,. CISCIIS. NIE. a-Dutvlene and Trans--butvlene.	This gas cell consists on a mixture of $_{2}$ O, $_{2}$ $_{2}$, $_{3}$, $_{2}$ $_{2}$, $_{3}$, $\alpha$ -Butylene and $\beta$ -butylene.
There are (wo main bands covering a significant fraction of the II-band (red vertical lines) which are not heavily affected by telluric absorptions and (thus make them object of interest for accurate velocity measurements.	There are two main bands covering a significant fraction of the H-band (red vertical lines) which are not heavily affected by telluric absorptions and thus make them object of interest for accurate velocity measurements.
The first one is clearly seen as a forest [rom 1.471.54 jan. mainly due to acetvlene absorption (53 lines resolved al 0.1 ! between mn: Ίου 66000) but also ammonia.	The first one is clearly seen as a forest from 1.47–1.54 $\mu$ m, mainly due to acetylene absorption (53 lines resolved at 0.1 $^{-1}$ between $\mu$ m; $\sim 66000$ ) but also ammonia.
Acetvlene was one of the first candidates and was already used	Acetylene was one of the first candidates and was already used
instead: based: purely. upon whether the periodic signal is persistent in time and frequency. and upon the shape of the pulse profile. with little or no indication of whether à source is actually terrestrial in origin.	instead based purely upon whether the periodic signal is persistent in time and frequency, and upon the shape of the pulse profile, with little or no indication of whether a source is actually terrestrial in origin.
This led to there being an overwhelming number of candidates. especially at low DM.	This led to there being an overwhelming number of candidates, especially at low DM.
A typical single beam from the survey would generate ~ 170 candidates. leading to à total of over 3.5 million candidates in the survey.	A typical single beam from the survey would generate $\sim$ 170 candidates, leading to a total of over 3.5 million candidates in the survey.
This large number of candidates is impossible to filter ov eve and so some automated filters were designed to reduce he number to be viewed.	This large number of candidates is impossible to filter by eye and so some automated filters were designed to reduce the number to be viewed.
As the MMD receiver has multiple »eanms. it allows us to compare each of the beams from the same observation. and assume that if à periodic signal is detected in many beams. then it is likely to be grouncd-based VL	As the MMB receiver has multiple beams, it allows us to compare each of the beams from the same observation, and assume that if a periodic signal is detected in many beams, then it is likely to be ground-based RFI.
Fherefore. any periodicities which appeared in two or more beams from the same pointing and had a period which matched within a tolerance of 10 ns were rejected.	Therefore, any periodicities which appeared in two or more beams from the same pointing and had a period which matched within a tolerance of 10 ns were rejected.
As shown in equation (4)). the S/N of a periodic signal decreases as the elfective pulse width increases for a given set of observing parameters.	As shown in equation \ref{senseq}) ), the S/N of a periodic signal decreases as the effective pulse width increases for a given set of observing parameters.
The effective width is given by where Wap is equal to the sampling rate and. 7; is a distortion in the pulse width due to scattering in the LSAL (given by equation (6))).	The effective width is given by where $W_{\mathrm{samp}}$ is equal to the sampling rate and $\tau_\mathrm{s}$ is a distortion in the pulse width due to scattering in the ISM (given by equation \ref{bhatscatter}) )).
Equation (3)) can be used to give Af. where Av is now the bandwidth of a single filterbank channel.	Equation \ref{dispersion}) ) can be used to give $\Delta t$, where $\Delta\nu$ is now the bandwidth of a single filterbank channel.
This broadening of the pulse arises due to the decispersion process and the finite width of the filterbank channels in the observing svstem.	This broadening of the pulse arises due to the dedispersion process and the finite width of the filterbank channels in the observing system.
Fig.	Fig.
G shows S/N against trial DAL error for signals with duty eveles of50%.. and it can be seen that S/N drops olf more quickly Xfor narrower pulses.	\ref{snr_vs_dm_w} shows S/N against trial DM error for signals with duty cycles of, and; it can be seen that S/N drops off more quickly for narrower pulses.
Fhus. a filter was applied. to the candidates to reject any with a width greater than of the period. which eliminated sinusoidal signals often indicative of REL which are often of high S/N for à very large range of trial DAIs.	Thus, a filter was applied to the candidates to reject any with a width greater than of the period, which eliminated sinusoidal signals often indicative of RFI, which are often of high S/N for a very large range of trial DMs.
In total. these two filters removed ~15% of the candidates from the processing pipeline.	In total, these two filters removed $\sim$ of the candidates from the processing pipeline.
During the inspection of the candidates. a further cut was made. removing all candidates with S/N κ 9.	During the inspection of the candidates, a further cut was made, removing all candidates with S/N $<$ 9.
This removed. a further of the candidates. with many of those remaining clustered around common REL frequencies.	This removed a further of the candidates, with many of those remaining clustered around common RFI frequencies.
]t is common. curing the inspection process. to visualise the candidates in. Period-DAL space (for an example using the JReaper software. soe Fig.	It is common, during the inspection process, to visualise the candidates in Period-DM space (for an example using the JReaper software, see Fig.
2 in 2)). so that any ‘clustering’ of the candidates at RET frequencies is highly apparent. making it easier for such candidates to be ignored.	2 in \citet{kel+09}) ), so that any `clustering' of the candidates at RFI frequencies is highly apparent, making it easier for such candidates to be ignored.
This reduced the number of candidates to 10000. and given that it takes only a few seconds to classify a cancidate. this allowed visual inspection of this subset of the survey output.	This reduced the number of candidates to $\sim10000$, and given that it takes only a few seconds to classify a candidate, this allowed visual inspection of this subset of the survey output.
The first. processing of the data. by2.. uncovered. one previously unknown pulsar. the voung and highly energetic PSR. 6132.	The first processing of the data, by\citet{obrien08}, uncovered one previously unknown pulsar, the young and highly energetic PSR $-$ 6132.
? noted that the pulsar was within the error box of the ECRET source 3E: 6147 and it is within that of the Fermi source 6128c (C2)..	\citet{obrien08} noted that the pulsar was within the error box of the EGRET source 3EG $-$ 6147 and it is within that of the Fermi source $-$ 6128c \citep{abdoetal}.
The pulsar is regularly observed at Parkes as part of the timing support for the Fermi mission (2).. but as vet pulsations in eamma-ravs have not been detected (?)..	The pulsar is regularly observed at Parkes as part of the timing support for the Fermi mission \citep{weltevrede2010}, but as yet pulsations in gamma-rays have not been detected \citep{fermipsrcat}.
One further pulsar. PSR 0812. with a period of 491 ms and a DM o£ 1023em?pe was discovered during the reprocessing of the Galactic-plane data (detailed in Section 77)).	One further pulsar, PSR $-$ 0812, with a period of 491 ms and a DM of $1023\,\mathrm{cm}^{-3}\,\mathrm{pc}$ was discovered during the reprocessing of the Galactic-plane data (detailed in Section \ref{sec:reprocessing}) ).
As seen in the top panel of Fig. Ἐν,	As seen in the top panel of Fig. \ref{1834prof},
the pulse profile αἱ 6.5 Gilg is narrow with a duty evele of only2:4... which ensured that the S/N was significantly lower away from the true value of DM. as shown in Fi .	the pulse profile at 6.5 GHz is narrow with a duty cycle of only, which ensured that the S/N was significantly lower away from the true value of DM, as shown in Fig. \ref{1834snrdm}.
The pulsar has been observed at a frequency of 4.85Giz using the IElfelsberg 100-m radio telescope. and at 1.4 Cillz with the Lovell telescope.	The pulsar has been observed at a frequency of $4.85\,\mathrm{GHz}$ using the Effelsberg 100-m radio telescope, and at 1.4 GHz with the Lovell telescope.
The profile is extremely. scatter broacdencd at this. frequency. with a scattering. time of 7150 ms.	The profile is extremely scatter broadened at this frequency, with a scattering time of $\sim$ 150 ms.
“Phe pulse profiles at 4.55 ancl 1.4 Cllz are shown in the bottom two panels of Fig. 7..	The pulse profiles at 4.85 and 1.4 GHz are shown in the bottom two panels of Fig. \ref{1834prof}.

This is interesting iu view of a determination of the total cnerey fiux along the jet (e.g. Celotti et al.

This is interesting in view of a determination of the total energy flux along the jet (e.g. Celotti et al.

1997. Sikora ct al.

1997, Sikora et al.

1997).

The total kinetic” power of the jet can be written as: where AR is the jet radius. D ds the bulk Lorentz factor aud Ü is the total energy deusitv in the jet. including radiation. magnetic field. relativistic particles aud eventually protous.

The total " kinetic" power of the jet can be written as: where $R$ is the jet radius, $\Gamma$ is the bulk Lorentz factor and $U$ is the total energy density in the jet, including radiation, magnetic field, relativistic particles and eventually protons.

If one assumes that there is 1 (cold) proton per relativistic electron. the proton contribution is usually dominant.

If one assumes that there is 1 (cold) proton per relativistic electron, the proton contribution is usually dominant.

Iu Fig.

In Fig.

2 the derived radiative huninosity £44 aud kinetic power of the jet Pia for a group of sources with sufficieutlv good spectral information are compared.

2 the derived radiative luminosity $L_{\rm jet}$ and kinetic power of the jet $P_{\rm jet}$ for a group of sources with sufficiently good spectral information are compared.

The ratio between these two quantities eives directly the "radiative efficiency? of the jet. which turis out to be jj20.1. though with large scatter.

The ratio between these two quantities gives directly the “radiative efficiency” of the jet, which turns out to be $\eta\simeq 0.1$, though with large scatter.

The line traces the result of a least-squares ft: we found a slope ~1.3. suggesting a decrease ofthe radiative efficiency. with decreasing power.

The line traces the result of a least-squares fit: we found a slope $\sim 1.3$, suggesting a decrease of the radiative efficiency with decreasing power.

Two iain classes of models for the production of jets has been proposed.

Two main classes of models for the production of jets has been proposed.

The frst class considers the extraction of rotational enerev from the black

The first class considers the extraction of rotational energy from the black

dashed lines uutil they eventually intersect the cooling inflow at some large radius r,..

dashed lines until they eventually intersect the cooling inflow at some large radius $r_c$.

audThe europe of the bubbles and flow are identical atr, the bubbles provide Bonjust chough gas to maintain the inflowing cooling flow that radius.

The entropy of the bubbles and flow are identical at $r_c$ and the bubbles provide just enough gas to maintain the inflowing cooling flow from that radius.

The third row of paucls(ο. aud. À) shows the uegative cooling inflow with solid lines aud he much faster outward motion of the riiug bubbles. ej>.0. with dashed lines.

The third row of panels, and ) shows the negative cooling inflow with solid lines and the much faster outward motion of the rising bubbles, $u_b > 0$, with dashed lines.

The variation of the bubble radius ois shown in thebottom row of panels(df aud 2 with dash- lines.

The variation of the bubble radius $r_b(r)$ is shown in the bottom row of panels, and ) with dash-dotted lines.

The dashed lines iu these bottom panels show the variation of the inflow volume filling factor f(r).

The dashed lines in these bottom panels show the variation of the inflow volume filling factor $f(r)$.

As h approaches the highest possible value for each bubble mass mp. ho» huyus thebubbles nearly fill the eutire available volume at kj where f0 0. as explained by Condition (21).

As $h$ approaches the highest possible value for each bubble mass $m_b$, $h \rightarrow h_{max}$ , the bubbles nearly fill the entire available volume at $r_h$ where $f \rightarrow 0$ , as explained by Condition (21).

For the most massive bubbles cousidered. ay,=LO A... solutions for two heating parameters are shown. )—3 and 6 for which the circulation radi are r,LO and 25 kpe respectively.

For the most massive bubbles considered, $m_b = 10^6$ $M_{\odot}$, solutions for two heating parameters are shown, $h = 3$ and 6 for which the circulation radii are $r_c = 10$ and 25 kpc respectively.

The deusity. temperature and velocity profiles for the cooling inflows for these two solutions are alinost ideutical.

The density, temperature and velocity profiles for the cooling inflows for these two solutions are almost identical.

We have not considered larger values of h because thebubble velocity «, for the f=6 solution the sound speed iu the cooling flow (50/3)?=ee(T/lO Klaus. |.

We have not considered larger values of $h$ because the bubble velocity $u_b$ for the $h = 6$ solution approaches the sound speed in the cooling flow $(5 \theta /3)^{1/2} = 476~(T/10^7~{\rm K})$ km $^{-1}$.

Larger / would result in supersonic bubble velocities that would drive shocks iuto the cooling eas. drsinatficallv increasing its temperature.

Larger $h$ would result in supersonic bubble velocities that would drive shocks into the cooling gas, dramatically increasing its temperature.

Also the bubble size attorj for the f=6 solution. η)~1 kpc Is Colmparable rp. again arene agaist larger values of h.

Also the bubble size at $r_h$ for the $h = 6$ solution, $r_b(r_h) \sim 1$ kpc is comparable to $r_h$, again arguing against larger values of $h$.

The ceutral column of Fiewe 2 illustrates two circulation flows forbubbles of mass me=Q0 AL. for h —3aud 6.5.

The central column of Figure 2 illustrates two circulation flows for bubbles of mass $m_b = 10^5$ $M_{\odot}$ for $h = 3$ and 6.5.

The circulation with —x6.5 extends out to =[8 kpc. but the flow fillime factor f less than abou Ll atory so there are uo circulations with fo6.5zchi, (Condition 21).

The circulation with $h = 6.5$ extends out to $r_c = 18$ kpc, but the flow filling factor $f$ is less than about 0.1at $r_h$ so there are no circulations with $h > 6.5 \approx h_{max}$ (Condition 21).

Iu order for this mareial flow to suppor unss flux M. the relative flow muo nuust as SOory, and the drag increases accordinely.

In order for this marginal flow to support mass flux ${\dot M}$ , the relative flow $u_b - u$ must increase as $r \rightarrow r_h$ and the drag increases accordingly.

The pirebubble velocity a, is secu to decline toward +).

The bubble velocity $u_b$ is seen to decline toward $r_h$.

As a result he laree drag. the effective eravity g,. (Equation 15) is directed outward near ry,lL kpe where the flow woul Ravleigh-Tavlor unstable.

As a result of the large drag, the effective gravity $g_e$ (Equation 15) is directed outward near $r_h = 1$ kpc where the flow would be Rayleigh-Taylor unstable.

This region of instability vecolmcs larger for higher values of 5.

This region of instability becomes larger for higher values of $h$.

Because of the approximations we have made. the deusitv in the flow region ry«or<r, is somewhat higher than the density observed iu NCC I172 (dotted lines).

Because of the approximations we have made, the density in the flow region $r_h < r < r_c$ is somewhat higher than the density observed in NGC 4472 (dotted lines).

However. if this flow were observed. the appareut density iyap, would be owered since the flow only occupies a fraction. f£ of the volume. Le. n,app!)29f2r).

However, if this flow were observed, the apparent density $n_{e,app}$ would be lowered since the flow only occupies a fraction $f$ of the volume, i.e., $n_{e,app}(r) \approx f^{1/2} n_e(r)$.

The frst cohuun in Fieure 2 shows the circulation ραίσα for bubbles of mass ney«10! AL. for two flows with h=3 aud

The first column in Figure 2 shows the circulation pattern for bubbles of mass $m_b = 3 \times 10^4$ $M_{\odot}$ for two flows with $h = 3$ and 3.6.

The flow fllius factor f is dropping rapidly as ro>ry for the f=3.6 solution so lis is close to the maximum possible heating (and 7.) for hese smallerbubbles.

The flow filling factor $f$ is dropping rapidly as $r \rightarrow r_h$ for the $h = 3.6$ solution so this is close to the maximum possible heating (and $r_c$ ) for these smaller bubbles.

We were unable to achieve fully convergent flow solutions with even sinallerbubbles of nass nn,S&SLO’ ALL.

We were unable to achieve fully convergent flow solutions with even smaller bubbles of mass $m_b \lta 10^4$ $M_{\odot}$ .

While our search for such solutions was not exhaustive. if is apparent from the trend im pauclsk »g > ein Figure 2 that the maximaun values of u;. 7 and r,. all decrease with my. as expected frou condition 22),

While our search for such solutions was not exhaustive, it is apparent from the trend in panels $\rightarrow$ $\rightarrow$ in Figure 2 that the maximum values of $u_b$, $h$ and $r_c$ all decrease with $m_b$, as expected from condition (22).

Bubbles of mass ai,=3<104 AL. are approaching the minima 25 necessary to carry the cooling mass flow AT foy auy heating 5h21.

Bubbles of mass $m_b = 3 \times 10^4$ $M_{\odot}$ are approaching the minimum $m_b$ necessary to carry the cooling mass flow ${\dot M}$ for any heating $h > 1$.

Nou-circulating flows with bubbles of lower mass must ultimately cool radiativelv to temperatures mich lower than Trj). iu disagreement with NADAL observations.

Non-circulating flows with bubbles of lower mass must ultimately cool radiatively to temperatures much lower than $T(r_h)$, in disagreement with XMM observations.

One of the motivations for our exploration of nou-rocks circulation flows is to estimate the influence of the bubbles on the apparent eas temperature which typically has a nuninuun near the origin.

One of the motivations for our exploration of non-cooling circulation flows is to estimate the influence of the bubbles on the apparent gas temperature which typically has a minimum near the origin.

To simulate the apparcut temperature that would be inferred when viewiug the cooling inflow aud the hot rising bubbles aloug the same lue of sight. we calculated the local cuission-weighted telpcrature which is plotted as dotted lines for each of the flows in panels5.f audj of Figure 2.

To simulate the apparent temperature that would be inferred when viewing the cooling inflow and the hot rising bubbles along the same line of sight, we calculated the local emission-weighted temperature which is plotted as dotted lines for each of the flows in panels, and of Figure 2.

For most circulation flows (7) is nearly iudistinguisliable frou the temperature of the cooling flow component.

For most circulation flows $\langle T\rangle$ is nearly indistinguishable from the temperature of the cooling flow component.

Consequcuth. a sinele phase interpretation of the temperature profile would show a mildly positive eradieut. dffdro>0. similar to those observed aud consisteut with traditional cooling flows.

Consequently, a single phase interpretation of the temperature profile would show a mildly positive gradient, $dT/dr > 0$, similar to those observed and consistent with traditional cooling flows.

This is a desirable feature of the circulation model.

Qu for the least iuassive bubbles cousidered. mdifferential«10! AL... does (P3 vise slightly as r>ry. but the change in the temperature profile caused by the hot bubbles is xnall.

Only for the least massive bubbles considered, $m_b = 3 \times 10^4$ $M_{\odot}$, does $\langle T\rangle$ rise slightly as $r \rightarrow r_h$, but the differential change in the temperature profile caused by the hot bubbles is small.

Tle apparent density pap)(C023)72. and eutropy profiles are also similar to those of the cooling flow component alouc.

The apparent density $\rho_{app} = (\langle \rho^2 \rangle)^{1/2}$ and entropy profiles are also similar to those of the cooling flow component alone.

We stress that these results differ from normal couvection where (1) there is a single temperature and density at every radius (apart from fluctuations). (2) the temperature eradieut is determined by the gravitational potential. dffdr=(270,ΕΙ fdr). aud theretore has a sig opposite to that observed. aud (3) the entropy is constant.

We stress that these results differ from normal convection where (1) there is a single temperature and density at every radius (apart from fluctuations), (2) the temperature gradient is determined by the gravitational potential, $dT/dr = -(2 \mu m_p/5 k)(d \Phi /dr)$ , and therefore has a sign opposite to that observed, and (3) the entropy is constant.

The ratio of Pd/V heating to drag heating is where a,«|e] appropriateand sve use qzzLAF«10Ln cms ? whichis for lXors 1003 NCC 1172.

The ratio of $PdV$ heating to drag heating is where $u_b \ll |u|$ and we use $g \approx 4.47 \times 10^{-7} r_{kpc}^{-0.85}$ cm $^{-2}$ which is appropriate for $1 \lta r_{kpc} \lta 100$ in NGC 4472.

The result Z,4;/2,471 follows nunediately frou Equation (13) provided dui, ΠΜ

The result ${\dot \varepsilon}_{pdv}/{\dot \varepsilon}_d \sim 1$ follows immediately from Equation (13) provided $u_b \ll |u|$.

of the uncertain physical nature of these two comparablebubble-flow heating mechanisimnis. we cousider heating due to bubble expansion and drag separately,

In view of the uncertain physical nature of these two comparable bubble-flow heating mechanisms, we consider heating due to bubble expansion and drag separately.

Figure 23 illustrates four represcutative cooling flow models in which the work done by the drag force is assuned to leat the local cooling flow eas with various efficiencies ο) (aud Cyd.= 0).

Figure 3 illustrates four representative cooling flow models in which the work done by the drag force is assumed to heat the local cooling flow gas with various efficiencies $e_d$ (and $e_{pdv} = 0$ ).

As before AT07 M. t and ry,=1d kpe for allflows.

As before ${\dot M} = 0.7$ $M_{\odot}$ $^{-1}$ and $r_h = 1$ kpc for allflows.

The fourflows also have the same bubble mass a,=10° M. and heating factor 5h=6. but thebubble drag heating cfiicieucy has values e,= 0. 0.1. 0.3 and0.7.

The fourflows also have the same bubble mass $m_b = 10^5$ $M_{\odot}$ and heating factor $h = 6$, but the bubble drag heating efficiency has values $e_d = 0$ , 0.1, 0.3 and0.7.

Flows with progressively lugher T. 75 aud » near the heating radius ky correspoud to increasing efficiencies.

Flows with progressively higher $T$, $T_b$ and $n$ near the heating radius $r_h$ correspond to increasing efficiencies.

By contrast. the circulation radii. velocitics.filling factors audbubble radii are inscusitive to the heating efficieucy.

By contrast, the circulation radii, velocities,filling factors and bubble radii are insensitive to the heating efficiency.

However. the flow with the largest heating efiicieucy. ο=OF is less satisfactory because flow teniperature aud particularly the appareut temperature(75 develop appreciable negative radial gradieuts ucar rj.

However, the flow with the largest heating efficiency, $e_d = 0.7$ is less satisfactory because flow temperature and particularly the apparent temperature$\langle T \rangle$ develop appreciable negative radial gradients near $r_h$ .

Because of

seven of them show neeligible absorption. or do not show any band or line so they. were discarded for the gas mixtures.

Seven of them show negligible absorption, or do not show any band or line so they were discarded for the gas mixtures.

We have chosen high puritv gases commercially. available with deeper absorptions and wider spectral coverage. adding and/or replacing individual eases with new ones. includiug acetvlene. nitrous oxide. hydrocarbons ancl chloromethans. using different partial pressures.

We have chosen high purity gases commercially available with deeper absorptions and wider spectral coverage, adding and/or replacing individual gases with new ones, including acetylene, nitrous oxide, hydrocarbons and chloromethans, using different partial pressures.

All of them are safe (ο use at this small concentrations. are nol corrosive and are gaseous al room temperature: (his makes (hem suitable for regular eround-based In total we have worked with five new different. mixtures (see Figure 5)).

All of them are safe to use at this small concentrations, are not corrosive and are gaseous at room temperature; this makes them suitable for regular ground-based In total we have worked with five new different mixtures (see Figure \ref{fig2}) ).

We have listed the composition in Table 4..

We have listed the composition in Table \ref{tab2}.

Due to the number of gas cells available. only three have been measured twice for stability. study.

Due to the number of gas cells available, only three have been measured twice for stability study.

The first two new mixtures (namely Mixture-I. 111. included nitrous oxide. acetvlene. methane and/or ehloromethans: only Mixture-I was measured on (wo occasions three months apart.

The first two new mixtures (namely Mixture-I, II), included nitrous oxide, acetylene, methane and/or chloromethans; only Mixture-I was measured on two occasions three months apart.

We found Mixture-I to be stable. with differences on the measurements lower than on band absorption intensity and nnm on line position.

We found Mixture-I to be stable, with differences on the measurements lower than on band absorption intensity and nm on line position.

Dased on (his mixture. three additional mixtures introducing ammonia and hydrocarbons were produced. namely NIL;i-I. HH: and HII.

Based on this mixture, three additional mixtures introducing ammonia and hydrocarbons were produced, namely $_{3}$ -I, II and III.

The mixture δα Π was measured eight months apart and remained stable with time ancl temperature. but we have discarded methane because of the atmospheric absorption.

The mixture $_{3}$ -II was measured eight months apart and remained stable with time and temperature, but we have discarded methane because of the atmospheric absorption.

We have carried ont a characterization of the NIL4-HI gas cell bv means of an Infrared Fourier Transform (FTIR) Spectrometer (Domen DAS). located at the University of Central Florida (USA).

We have carried out a characterization of the $_{3}$ -III gas cell by means of an Infrared Fourier Transform (FTIR) Spectrometer (Bomen DA8), located at the University of Central Florida (USA).

The instrument makes use of a InSb (€ Indium Antimonice) detector. a cquartz-halogen lamp as source and a quartz beam-splitter.

The instrument makes use of a InSb ( Indium Antimonide) detector, a quartz-halogen lamp as source and a quartz beam-splitter.

The spectrum was obtained wider vacuum (< 5mTorr) at 23°C with a resolution of 0.1 + (R = 40000 at 2.5 jm).

The spectrum was obtained under vacuum $<$ 5mTorr) at $\degr$ C with a resolution of 0.1 $^{-1}$ (R = 40000 at 2.5 $\mu$ m).

The cell was measured with Cary 5 and on two separate occasions wilh FTIR. three and eight months apart.

The cell was measured with Cary 5 and on two separate occasions with FTIR three and eight months apart.

Figure ?? compares a high resolution measurement with the low resolution measurement. an ammonia gas cell NIL, + Argon). a M9 brown dwar moclel (I. ~ 65000) and a telluric spectra in absorption (from top to bottom).

Figure \ref{3} compares a high resolution measurement with the low resolution measurement, an ammonia gas cell $_{3}$ + Argon), a M9 brown dwarf model (R $\sim 65000$ ) and a telluric spectra in absorption (from top to bottom).

This gas cell consists on a mixture of NoO. Πο, CICIL,. CISCIIS. NIE. a-Dutvlene and Trans--butvlene.

This gas cell consists on a mixture of $_{2}$ O, $_{2}$ $_{2}$, $_{3}$, $_{2}$ $_{2}$, $_{3}$, $\alpha$ -Butylene and $\beta$ -butylene.

There are (wo main bands covering a significant fraction of the II-band (red vertical lines) which are not heavily affected by telluric absorptions and (thus make them object of interest for accurate velocity measurements.

There are two main bands covering a significant fraction of the H-band (red vertical lines) which are not heavily affected by telluric absorptions and thus make them object of interest for accurate velocity measurements.

The first one is clearly seen as a forest [rom 1.471.54 jan. mainly due to acetvlene absorption (53 lines resolved al 0.1 ! between mn: Ίου 66000) but also ammonia.

The first one is clearly seen as a forest from 1.47–1.54 $\mu$ m, mainly due to acetylene absorption (53 lines resolved at 0.1 $^{-1}$ between $\mu$ m; $\sim 66000$ ) but also ammonia.

Acetvlene was one of the first candidates and was already used

Acetylene was one of the first candidates and was already used

instead: based: purely. upon whether the periodic signal is persistent in time and frequency. and upon the shape of the pulse profile. with little or no indication of whether à source is actually terrestrial in origin.

instead based purely upon whether the periodic signal is persistent in time and frequency, and upon the shape of the pulse profile, with little or no indication of whether a source is actually terrestrial in origin.

This led to there being an overwhelming number of candidates. especially at low DM.

This led to there being an overwhelming number of candidates, especially at low DM.

A typical single beam from the survey would generate ~ 170 candidates. leading to à total of over 3.5 million candidates in the survey.

A typical single beam from the survey would generate $\sim$ 170 candidates, leading to a total of over 3.5 million candidates in the survey.

This large number of candidates is impossible to filter ov eve and so some automated filters were designed to reduce he number to be viewed.

This large number of candidates is impossible to filter by eye and so some automated filters were designed to reduce the number to be viewed.

As the MMD receiver has multiple »eanms. it allows us to compare each of the beams from the same observation. and assume that if à periodic signal is detected in many beams. then it is likely to be grouncd-based VL

As the MMB receiver has multiple beams, it allows us to compare each of the beams from the same observation, and assume that if a periodic signal is detected in many beams, then it is likely to be ground-based RFI.

Fherefore. any periodicities which appeared in two or more beams from the same pointing and had a period which matched within a tolerance of 10 ns were rejected.

Therefore, any periodicities which appeared in two or more beams from the same pointing and had a period which matched within a tolerance of 10 ns were rejected.

As shown in equation (4)). the S/N of a periodic signal decreases as the elfective pulse width increases for a given set of observing parameters.

As shown in equation \ref{senseq}) ), the S/N of a periodic signal decreases as the effective pulse width increases for a given set of observing parameters.

The effective width is given by where Wap is equal to the sampling rate and. 7; is a distortion in the pulse width due to scattering in the LSAL (given by equation (6))).

The effective width is given by where $W_{\mathrm{samp}}$ is equal to the sampling rate and $\tau_\mathrm{s}$ is a distortion in the pulse width due to scattering in the ISM (given by equation \ref{bhatscatter}) )).

Equation (3)) can be used to give Af. where Av is now the bandwidth of a single filterbank channel.

Equation \ref{dispersion}) ) can be used to give $\Delta t$, where $\Delta\nu$ is now the bandwidth of a single filterbank channel.

This broadening of the pulse arises due to the decispersion process and the finite width of the filterbank channels in the observing svstem.

This broadening of the pulse arises due to the dedispersion process and the finite width of the filterbank channels in the observing system.

Fig.

G shows S/N against trial DAL error for signals with duty eveles of50%.. and it can be seen that S/N drops olf more quickly Xfor narrower pulses.

\ref{snr_vs_dm_w} shows S/N against trial DM error for signals with duty cycles of, and; it can be seen that S/N drops off more quickly for narrower pulses.

Fhus. a filter was applied. to the candidates to reject any with a width greater than of the period. which eliminated sinusoidal signals often indicative of REL which are often of high S/N for à very large range of trial DAIs.

Thus, a filter was applied to the candidates to reject any with a width greater than of the period, which eliminated sinusoidal signals often indicative of RFI, which are often of high S/N for a very large range of trial DMs.

In total. these two filters removed ~15% of the candidates from the processing pipeline.

In total, these two filters removed $\sim$ of the candidates from the processing pipeline.

During the inspection of the candidates. a further cut was made. removing all candidates with S/N κ 9.

During the inspection of the candidates, a further cut was made, removing all candidates with S/N $<$ 9.

This removed. a further of the candidates. with many of those remaining clustered around common REL frequencies.

This removed a further of the candidates, with many of those remaining clustered around common RFI frequencies.

]t is common. curing the inspection process. to visualise the candidates in. Period-DAL space (for an example using the JReaper software. soe Fig.

It is common, during the inspection process, to visualise the candidates in Period-DM space (for an example using the JReaper software, see Fig.

2 in 2)). so that any ‘clustering’ of the candidates at RET frequencies is highly apparent. making it easier for such candidates to be ignored.

2 in \citet{kel+09}) ), so that any `clustering' of the candidates at RFI frequencies is highly apparent, making it easier for such candidates to be ignored.

This reduced the number of candidates to 10000. and given that it takes only a few seconds to classify a cancidate. this allowed visual inspection of this subset of the survey output.

This reduced the number of candidates to $\sim10000$, and given that it takes only a few seconds to classify a candidate, this allowed visual inspection of this subset of the survey output.

The first. processing of the data. by2.. uncovered. one previously unknown pulsar. the voung and highly energetic PSR. 6132.

The first processing of the data, by\citet{obrien08}, uncovered one previously unknown pulsar, the young and highly energetic PSR $-$ 6132.

? noted that the pulsar was within the error box of the ECRET source 3E: 6147 and it is within that of the Fermi source 6128c (C2)..

\citet{obrien08} noted that the pulsar was within the error box of the EGRET source 3EG $-$ 6147 and it is within that of the Fermi source $-$ 6128c \citep{abdoetal}.

The pulsar is regularly observed at Parkes as part of the timing support for the Fermi mission (2).. but as vet pulsations in eamma-ravs have not been detected (?)..

The pulsar is regularly observed at Parkes as part of the timing support for the Fermi mission \citep{weltevrede2010}, but as yet pulsations in gamma-rays have not been detected \citep{fermipsrcat}.

One further pulsar. PSR 0812. with a period of 491 ms and a DM o£ 1023em?pe was discovered during the reprocessing of the Galactic-plane data (detailed in Section 77)).

One further pulsar, PSR $-$ 0812, with a period of 491 ms and a DM of $1023\,\mathrm{cm}^{-3}\,\mathrm{pc}$ was discovered during the reprocessing of the Galactic-plane data (detailed in Section \ref{sec:reprocessing}) ).

As seen in the top panel of Fig. Ἐν,

As seen in the top panel of Fig. \ref{1834prof},

the pulse profile αἱ 6.5 Gilg is narrow with a duty evele of only2:4... which ensured that the S/N was significantly lower away from the true value of DM. as shown in Fi .

the pulse profile at 6.5 GHz is narrow with a duty cycle of only, which ensured that the S/N was significantly lower away from the true value of DM, as shown in Fig. \ref{1834snrdm}.

The pulsar has been observed at a frequency of 4.85Giz using the IElfelsberg 100-m radio telescope. and at 1.4 Cillz with the Lovell telescope.

The pulsar has been observed at a frequency of $4.85\,\mathrm{GHz}$ using the Effelsberg 100-m radio telescope, and at 1.4 GHz with the Lovell telescope.

The profile is extremely. scatter broacdencd at this. frequency. with a scattering. time of 7150 ms.

The profile is extremely scatter broadened at this frequency, with a scattering time of $\sim$ 150 ms.

“Phe pulse profiles at 4.55 ancl 1.4 Cllz are shown in the bottom two panels of Fig. 7..

The pulse profiles at 4.85 and 1.4 GHz are shown in the bottom two panels of Fig. \ref{1834prof}.