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Since this οποιο” task was deemed to be vital for SRG, the satellite Principal Investigator required TAUVEX to be equipped with a BBF filter in every telescope of the three it carried. albeit its scientie value was not expected to be sienificant. | Since this “guiding” task was deemed to be vital for SRG, the satellite Principal Investigator required TAUVEX to be equipped with a BBF filter in every telescope of the three it carried, albeit its scientific value was not expected to be significant. |
The configurationC» of three telescopes within a cvlindcr. conceived for an OFEO lanuch. could not be maintained with TAUVEX ποιος on top of SODART at the space end of SRO. | The configuration of three telescopes within a cylinder, conceived for an OFEQ launch, could not be maintained with TAUVEX mounted on top of SODART at the space end of SRG. |
For this reason. the planned cevlindrical configuration was "unmwrapped and the three telescopes were designed to be almost. coplanar. | For this reason, the planned cylindrical configuration was “unwrapped” and the three telescopes were designed to be almost coplanar. |
The pavload was designed to fit iuto two units: an optical unit (OU) consisting of the mirrors, detectors, filter assemblies. ancl pre-aiplificr boards, aud an electronic unit (EU) of consistingthe power conditioning unit. analog-to-digital front ends. high-voltage power supplies, doubly-redundaut CPUs, on-board memory in the form of four 51 MD laptop hard disks in pressurized enclosures. ete. | The payload was designed to fit into two units: an optical unit (OU) consisting of the mirrors, detectors, filter assemblies, and pre-amplifier boards, and an electronic unit (EU) consisting of the power conditioning unit, analog-to-digital front ends, high-voltage power supplies, doubly-redundant CPUs, on-board memory in the form of four 84 MB laptop hard disks in pressurized enclosures, etc. |
This configuration was described by Topaz et al ( | This configuration was described by Topaz et al. ( |
1993), Schnopper (1991). Drosch et al. ( | 1993), Schnopper (1994), Brosch et al. ( |
199D), and. Leibowitz (1995). | 1994), and Leibowitz (1995). |
ISA aud Isvacl’s minister of Science and Technology (at that time the late Prof. Yuval οολα) issued w the cud of 1991 a letter to Prof. Rashid Suuvaev he SRO Principal Livestigator promising to deliver TAUVEN o the SRC spacecraft on time. according o the satellite schedule. | ISA and Israel's minister of Science and Technology (at that time the late Prof. Yuval Ne'eman) issued by the end of 1991 a letter to Prof. Rashid Sunyaev the SRG Principal Investigator promising to deliver TAUVEX to the SRG spacecraft on time, according to the satellite schedule. |
At this time. the plan was o launch SRC by 1991. | At this time, the plan was to launch SRG by 1994. |
With the conuuitinent to aunch on SRC. a contract was signed between ISA and the Ministry of Science and Technology on the one hand. and ELOp on the other hand. to provide he TAUVEN pavload according to previously agrecd-upon specifications. | With the commitment to launch on SRG, a contract was signed between ISA and the Ministry of Science and Technology on the one hand, and El-Op on the other hand, to provide the TAUVEX payload according to previously agreed-upon specifications. |
The investigator team at Tel Aviv University was to provide an advisory role in the xoject, with the final decisions to be taken by ISA. | The investigator team at Tel Aviv University was to provide an advisory role in the project, with the final decisions to be taken by ISA. |
Civen the short time table. the design of TAUVEX and its construction were performed iu record time » ELOp. and the project never iissed anv SRC nilestone. | Given the short time table, the design of TAUVEX and its construction were performed in record time by El-Op, and the project never missed any SRG milestone. |
This included the delivery of size and mass nodels aud of a thermal model (TAQ), ideutical in shape o the fight model (FM) but equipped with iuauxv sensors so that it could fully sinulate the behavior of TAUVEN in space couditions. | This included the delivery of size and mass models and of a thermal model (TM), identical in shape to the flight model (FM) but equipped with many sensors so that it could fully simulate the behavior of TAUVEX in space conditions. |
Prior to its delivery o Lavotchkin, the TAUVEN TAL undertook a full space simulation at the iABC facility in Coria. where a themmalvactuun chamber equipped with a solar simulator was used. | Prior to its delivery to Lavotchkin, the TAUVEX TM undertook a full space simulation at the iABG facility in Germany, where a thermal-vacuum chamber equipped with a solar simulator was used. |
Note also that the pressure to launch in time required the asseiuüblv of the flight OU to take place already in 1993. with detectors fabricated in 1992. | Note also that the pressure to launch in time required the assembly of the flight OU to take place already in 1993, with detectors fabricated in 1992. |
However, the dissolution of the Soviet Union brought about financial difficulties in Russia which inherited most of the Soviet space programs. | However, the dissolution of the Soviet Union brought about financial difficulties in Russia which inherited most of the Soviet space programs. |
In particular, SRC suffered continuous delavs and caused additional costs to the TAUVEN project. | In particular, SRG suffered continuous delays and caused additional costs to the TAUVEX project. |
Parcuthetically note that SRO has not vet )oeni launched. by 2010. althoueh it is still nanifested as a Russian Space Ageucy (RIA) nuission albeit with a different set of instruments. | Parenthetically, note that SRG has not yet been launched by 2010, although it is still manifested as a Russian Space Agency (RKA) mission albeit with a different set of instruments. |
Civeu the interminable delays, and the uncertainty that SRO would ever launch. ISA instructed the TAUVEX science team in 2000 to search for an alternate launch possibility. | Given the interminable delays, and the uncertainty that SRG would ever launch, ISA instructed the TAUVEX science team in 2000 to search for an alternate launch possibility. |
À launch alternativo was possible since TAUVEN was designed fom tle outset o require only mechanical fixation points. electrical power supply aud uplink/downliuk telemetry from anv platform it would be attached to. | A launch alternative was possible since TAUVEX was designed from the outset to require only mechanical fixation points, electrical power supply and uplink/downlink telemetry from any platform it would be attached to. |
where ζωΠόπη>. corresponds to the central temperature that the laver would need to have without compression (1.e.. for l=1). | where $k_B T_{\rm eq}\equiv B_0^2/16\pi n_0$ corresponds to the central temperature that the layer would need to have without compression (i.e., for $A=1$ ). |
This temperature can also be written in a convenient dimensionless form as IA — | This temperature can also be written in a convenient dimensionless form as _e = =. |
substituting this expression for the temperature into equation (2.3)). we gel (eoe)ο | Substituting this expression for the temperature into equation \ref{eq-Spitzer-S}) ), we get S_0 = _e) = = = )^4. |
Correspondingly, the reconnection velocity (2.2)) is given by(CB)(pen and the the thiekness of the laver (2.2)) becomes o7> pun| .CLr.) | Correspondingly, the reconnection velocity \ref{eq-v_rec-A2}) ) is given by, and the the thickness of the layer \ref{eq-delta}) ) becomes ^2 (L r_e) = 8 (L |
follows: being Q=νο. | follows: being $\mathcal{Q} \equiv \meanf{\narrowband}/\meanf{\broadband}$. |
The color of a source (wilh the color normalization of Sect. 2)) | The color of a source (with the color normalization of Sect. \ref{sec:description}) ) |
is directlv mg—mN2.5logQ. | is directly $m_{\broadband} -
m_{\narrowband} = 2.5 \log \mathcal{Q}$. |
Equation 22 shows that the EW does not change linearly with Q. | Equation \ref{eq:def:ew}
shows that the EW does not change linearly with $\mathcal{Q}$. |
There exists an upper limit to the color that a source can have due to the presence of an emission line: It is worth noting that observing an emission-line object with a narrow-band filler increases the contrast between the emission line and the continuum. as the object is brighter in (he line than in the continuum. | There exists an upper limit to the color that a source can have due to the presence of an emission line: It is worth noting that observing an emission-line object with a narrow-band filter increases the contrast between the emission line and the continuum, as the object is brighter in the line than in the continuum. |
Let us assume that we have two objects with the same magnitude in the broad-band. one wil line of equivalent width V (named L) ancl the other without emission (denoted C). | Let us assume that we have two objects with the same magnitude in the broad-band, one with line of equivalent width $W$ (named L) and the other without emission (denoted C). |
The ratio of the fluxes of the two objects measured in the narrow-band filter is (he contrast parameter. defined originally bv ?.. | The ratio of the fluxes of the two objects measured in the narrow-band filter is the contrast parameter, defined originally by \citet{1995AJ....110..963T}. |
Using Eq. 9.. | Using Eq. \ref{eq:flujo2}, |
we obtain: In the original contrast parameter of ?.. the width of the filter is characterized by its FWIIM. | we obtain: In the original contrast parameter of \citet{1995AJ....110..963T}, the width of the filter is characterized by its FWHM. |
For our Eq. | For our Eq. |
24 we. more accurately. use the effective width as defined in Eq. 7.. | \ref{eq:contraste} we, more accurately, use the effective width as defined in Eq. \ref{eq:def:ewidth}. |
The nuneric expression of the contrast parameter is equal to the equation obtained by inverting Eq. 22.. | The numeric expression of the contrast parameter is equal to the equation obtained by inverting Eq. \ref{eq:def:ew}. |
There are two limit cases for these equations. | There are two limit cases for these equations. |
When (he width of the broad-band is much greater than (he narrow-band width. we can consider that the line do not contribute to (he broad-band filter. | When the width of the broad-band is much greater than the narrow-band width, we can consider that the line do not contribute to the broad-band filter. |
The parameter € tends to zero and the equations can be written as: | The parameter $\epsilon$ tends to zero and the equations can be written as: |
spinning neutron stars. | spinning neutron stars. |
Fora predic35M. progenitor (the highest mass they considered). they that the neutron star will have a spin period of ms which is rapid enough for the generation of a a magnetar-type3 field by the αd dynamo mechanism of Duncan&"Thompson(1992). | For a $35\Msun$ progenitor (the highest mass they considered), they predict that the neutron star will have a spin period of $3$ ms which is rapid enough for the generation of a a magnetar-type field by the $\alpha-\omega$ dynamo mechanism of \citet{Duncan92}. |
. Llowever. for this to be a viable explanation of the magnetars. the aw dvnamo mechanism would need to be effective for neutron stars that arise from. progenitors with significantly: lower masses (20. 22M.) or the derived birthrate of magnetars would be too low to explain the observations. | However, for this to be a viable explanation of the magnetars, the $\alpha-\omega$ dynamo mechanism would need to be effective for neutron stars that arise from progenitors with significantly lower masses $\sim 20-22\Msun$ ) or the derived birthrate of magnetars would be too low to explain the observations. |
Furthermore. since the calculations of Legeretal.(2005) have been seriously challenged by Zahnctal.(2007)... it appears that we are still waiting for more stellar evolution calculations. that allow for both magneic Lickel and rotation. to show us whether or not millisecond rotation periods can result from massive stars. | Furthermore, since the calculations of \citet{Heger05} have been seriously challenged by \citet{Zahn07}, it appears that we are still waiting for more stellar evolution calculations, that allow for both magnetic field and rotation, to show us whether or not millisecond rotation periods can result from massive stars. |
Hf such. periods can be achieved. this wou give support to the idea that the dynamo mocel is a viab alternative to the fossil field hypothesis. although it is likeA hat a fossil field could still play the role of a seed field. | If such periods can be achieved, this would give support to the idea that the dynamo model is a viable alternative to the fossil field hypothesis, although it is likely that a fossil field could still play the role of a seed field. |
Lt is relevant that we comment on the alternative to our basic hypothesis on spin evolution. namely that the fick hat decays is also the field that drives spin evolution during he magnetar phase. | It is relevant that we comment on the alternative to our basic hypothesis on spin evolution, namely that the field that decays is also the field that drives spin evolution during the magnetar phase. |
We have considered. this possibility using “Avenue C7 of Colpi.Geppert.&Page(2000)... bu excluded it from our present considerations because it [aile o populate the high field end of the observed magnetar fiel distribution. | We have considered this possibility using “Avenue C” of \citet{Colpi00}, but excluded it from our present considerations because it failed to populate the high field end of the observed magnetar field distribution. |
It is conceivable that with the use of dilleren ield decay. parameters for avenue C we may also be able to mocel the data. but we expect that such a model will necc o have field characteristics during the magnetar phase tha are so similar to those adopted in the present caleulations hat our major conclusions will remain largely unchanged. | It is conceivable that with the use of different field decay parameters for avenue C we may also be able to model the data, but we expect that such a model will need to have field characteristics during the magnetar phase that are so similar to those adopted in the present calculations that our major conclusions will remain largely unchanged. |
In conclusion. we note that the origin of the crusta ied. component. in magnetars remains unresolved. | In conclusion, we note that the origin of the crustal field component in magnetars remains unresolved. |
Zahnetal.(2007). have shown that the shearing of a poloida ield of fossil origin in a clillerentially rotating radiative region can lead to the generation of a toroidal field so that ield. complexity of the type that appears to be required in nmagnetars may arise naturally from stellar evolution. when he complex interplay between rotation and fossil magnetic icles is taken into consideration. | \citet{Zahn07} have shown that the shearing of a poloidal field of fossil origin in a differentially rotating radiative region can lead to the generation of a toroidal field so that field complexity of the type that appears to be required in magnetars may arise naturally from stellar evolution, when the complex interplay between rotation and fossil magnetic fields is taken into consideration. |
On the other hand. since all-back discs are expected to play a role in the evolution of stars in the mass range 3045M... it is tempting to speculate that the crustal field component that characterises he magnetars may have its origin in the interaction of the all-back clise with the magnetic field of the stellar core. in cases where a magnetar is the outcome of stellar evolution. | On the other hand, since fall-back discs are expected to play a role in the evolution of stars in the mass range $\sim 20 - 45\Msun$, it is tempting to speculate that the crustal field component that characterises the magnetars may have its origin in the interaction of the fall-back disc with the magnetic field of the stellar core, in cases where a magnetar is the outcome of stellar evolution. |
If this is the case. one would expect that most of the mass in the fall-back clise would be magnetically ejected. | If this is the case, one would expect that most of the mass in the fall-back disc would be magnetically ejected. |
The authors would like to thank the Referee. U. Geppoert. for valuable comments and Ixoji Mukai for providing assistance with the ROSAT/PSPC X-ray selection software. | The authors would like to thank the Referee, U. Geppert, for valuable comments and Koji Mukai for providing assistance with the ROSAT/PSPC X-ray selection software. |
to the data of Kinet. spanning a range of Limagnitudes. | to the data of $^{\rm {1}}$, spanning a range of 4 magnitudes. |
These are shown iu the left pancl of Fig. | These are shown in the left panel of Fig. |
{ on a semi-log plot. with the xaxis iu arc seconds; | \ref{synthetic} on a semi-log plot, with the x–axis in arc seconds. |
We then applied a commuon saturation limit’ to all profiles to ης the saturation level of the photographic emulsion. aud resampled the data to a 5.25 arc second pixel size. | We then applied a common `saturation limit' to all profiles to mimic the saturation level of the photographic emulsion, and resampled the data to a 5.25 arc second pixel size. |
The welt haud paucl of Fig. | The right hand panel of Fig. |
E. shows the resulting profiles. | \ref{synthetic} shows the resulting profiles. |
The radius of saturation varies from around 2 to 13 pixels. | The radius of saturation varies from around 2 to 13 pixels. |
As explained below. the saturation intensity level was chosen so that the resulting radii of saturation matched the observed values from the plate scans. | As explained below, the saturation intensity level was chosen so that the resulting radii of saturation matched the observed values from the plate scans. |
We stress that the ouly adjustable paralucter in this matching is the choice of saturation inteusity level. ancl this is applied to all the svuthetic profiles. | We stress that the only adjustable parameter in this matching is the choice of saturation intensity level, and this is applied to all the synthetic profiles. |
Fig. | Fig. |
5 shows. as open circles. the measured radii of saturation for our 19 field stars. ranging from D—9 to ~13. | \ref{radius_comp} shows, as open circles, the measured radii of saturation for our 19 field stars, ranging from $\sim$ 9 to $\sim$ 13. |
We measured radii on 6 digitised plates whose plate maeuitudes were close to the eusemble moean deteziined from 90 plates. and then took averages for cach star. | We measured radii on 6 digitised plates whose plate magnitudes were close to the ensemble mean determined from 90 plates, and then took averages for each star. |
This procedure should minimise possible changes in stellar profiles caused by instrumental changes made during the survey. | This procedure should minimise possible changes in stellar profiles caused by instrumental changes made during the survey. |
The calculated radii of saturation of the svuthetic profiles of Fig. | The calculated radii of saturation of the synthetic profiles of Fig. |
1 are represcuted by the solid line. | \ref{synthetic} are represented by the solid line. |
We adjusted the common saturation level for | We adjusted the common saturation level for |
The Galaxy is observed to have a “boxy” bulge in near-infrared images (Dwek ct al. | The Galaxy is observed to have a “boxy” bulge in near-infrared images (Dwek et al. |
1995) and the nature and the origin” of the inner triaxiala shape of the Galaxy NE(1... bar/bulge) has been extensively discussedmM by several authors (c.g. Dabusiaux. Gilmore» 2005: Rattenbury et al. | 1995) and the nature and the origin of the inner triaxial shape of the Galaxy (i.e., bar/bulge) has been extensively discussed by several authors (e.g., Babusiaux Gilmore 2005; Rattenbury et al. |
2007). | 2007). |
- Recent spectroscopic observations on stellar abundances and kinematics of the Galactic bulge have provided new clues to he origin of the triaxial bulge (c.g... Melénndez et al. | Recent spectroscopic observations on stellar abundances and kinematics of the Galactic bulge have provided new clues to the origin of the triaxial bulge (e.g., Melénndez et al. |
2008: Zoccali οἱ al. | 2008; Zoccali et al. |
2008: Babusiaux et al. | 2008; Babusiaux et al. |
2010). | 2010). |
Melénadez οἱ al. ( | Melénndez et al. ( |
2008) found no/little differenees in chemical abundances of⋅ stars between the Galactic. bulge and the thick. disk and accordingly suggested a similar chemical evolution history tween the two components of the Galaxy. (see also Lace et al. | 2008) found no/little differences in chemical abundances of stars between the Galactic bulge and the thick disk and accordingly suggested a similar chemical evolution history between the two components of the Galaxy (see also Ryde et al. |
2010. Alves-Drito et al. | 2010, Alves-Brito et al. |
2010). | 2010). |
Zocalli οἱ al. ( | Zocalli et al. ( |
2008) ound a steep metallicity gradient along the minor axis of he bulge and suggested that the presence of the vertical | 2008) found a steep metallicity gradient along the minor axis of the bulge and suggested that the presence of the vertical |
this distance m terms of the pressure of the Jet at a reference position zo (Pio). which will be taken as the injection point in the grid. and the pressure of the ambient medium (P4). | this distance in terms of the pressure of the jet at a reference position $z_0$ $P_{\rm j,0}$ ), which will be taken as the injection point in the grid, and the pressure of the ambient medium $P_{\rm ext}$ ). |
From Eq. (1): | From Eq. \ref{eq:pres}) ): |
From this. certain limits on the pressure (and temperature) of jets. suitable to develop recollimation shocks. can be given. | From this, certain limits on the pressure (and temperature) of jets, suitable to develop recollimation shocks, can be given. |
Since we are interested in the region of maximal wind/jet interaction. we impose that the right hand side of the inequality in Eq. (2) | Since we are interested in the region of maximal wind/jet interaction, we impose that the right hand side of the inequality in Eq. \ref{eq:zxoc}) ) |
is €10 em. being a safe estimate for z,«Row. | is $\leq 10^{12}\,\rm{cm}$ , being a safe estimate for $z_{\rm s}<R_{\rm orb}$. |
Thus. fixing zo. an estimate of the initial overpressure in the jet that may result in a recollimation shock in<R4 can be given. | Thus, fixing $z_0$, an estimate of the initial overpressure in the jet that may result in a recollimation shock in$<R_{\rm orb}$ can be given. |
technique using X7 tests of phase-dispersion minimisation. | technique using $\chi^2$ tests of phase-dispersion minimisation. |
Each Πο curve with more than 1000 data points was analysed for cach object ou a per camera basis (to niunmnüse the effect of svstematic differences between different cameras). and imuultiple significant periods (iu sole cases} were identified for each. | Each light curve with more than 1000 data points was analysed for each object on a per camera basis (to minimise the effect of systematic differences between different cameras), and multiple significant periods (in some cases) were identified for each. |
The SuperWaAsP input catalogue is based on the USNO-DBI.O saple of over l billion stars. which extends down ο 1naenitude Von21. | The SuperWASP input catalogue is based on the USNO-B1.0 sample of over 1 billion stars, which extends down to magnitude $V \sim 21$. |
Tlowever. because the SuperWASP pixels are large (around 1 ") it is sometimes the case that multiple SuperWASP object apertures (each based ou the position of a single USNO-BI.O star) sample the variability from a siugle object. | However, because the SuperWASP pixels are large (around $14^{\prime\prime}$ ) it is sometimes the case that multiple SuperWASP object apertures (each based on the position of a single USNO-B1.0 star) sample the variability from a single object. |
This can result in iuItiple. closely spaced SuperWASP objects displaving the same periodic signal. | This can result in multiple, closely spaced SuperWASP objects displaying the same periodic signal. |
Also. despite using the SysRem algorithlin (Tammuz ct al. | Also, despite using the SysRem algorithm (Tamuz et al. |
2005) to reduce systematic contaminants in the liebt curves. If is apparent that may spurious periodic signals remain. particularly at harmonics of dl sidereal dav (νο, at periods of 1 sidercal dav/n where »=2.3.L...20. ete). | 2005) to reduce systematic contaminants in the light curves, it is apparent that many spurious periodic signals remain, particularly at harmonics of 1 sidereal day (i.e. at periods of 1 sidereal $n$ where $n=2,3,4...20,$ etc.). |
Period ranges within about a imuinute either side of these harmonics were therefore flageed as ikely spurious in the ialysis. | Period ranges within about a minute either side of these harmonics were therefore flagged as likely spurious in the analysis. |
This exercise viclded around 5.600 periodic signals iu the period range from about 125 minutes to 167 miüuutes (0.087 d to 0.116 d). excluding those ooriod ranges close to 1/9 d (€160 minutes). 1/10 d (—Ll nunutes) aud 1/11 d (~131 ος). | This exercise yielded around 5,600 periodic signals in the period range from about 125 minutes to 167 minutes (0.087 d to 0.116 d), excluding those period ranges close to 1/9 d $\sim 160$ minutes), 1/10 d $\sim 144$ minutes) and 1/11 d $\sim 131$ minutes). |
A further 17.300 periodic signals were identified close to 1/9 d: 11.500 signals close to 1/10 d: and 9.300 signals close to 1/11d. | A further 17,300 periodic signals were identified close to 1/9 d; 14,500 signals close to 1/10 d; and 9,300 signals close to 1/11d. |
The distribution of the ΠΙΟ of objects as a function of period within this range is shown iu Figure 1. | The distribution of the number of objects as a function of period within this range is shown in Figure 1. |
Note that a single variable object may give rise to multiple signals if it is observed o» anultiple cameras. or if the variability is sampled x multiple apertures correspoucding to closcly separated stars m the iuput catalogue. | Note that a single variable object may give rise to multiple signals if it is observed by multiple cameras, or if the variability is sampled by multiple apertures corresponding to closely separated stars in the input catalogue. |
Hence there are fewer unique xiodie objects iu this period range than indicated by the nunbers quoted above. | Hence there are fewer unique periodic objects in this period range than indicated by the numbers quoted above. |
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