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This means that a smooth change of £. namely D. at the critical point is the essential requirement for a (raus-magnetosonic flow.) | This means that a smooth change of $\xi$, namely $B_\phi$, at the critical point is the essential requirement for a trans-magnetosonic flow.) |
Thus. we can obtain a trans-last magnetosonie [low solution without the regularity condition at the fast maegnetosonic point. | Thus, we can obtain a trans-fast magnetosonic flow solution without the regularity condition at the fast magnetosonic point. |
The behavior of the acceleration in the outgoing flow is determined by &=€Cr). andl the asymptotic feature depends on the value o£ £: that is. €> or £<&.. | The behavior of the acceleration in the outgoing flow is determined by $\xi=\xi(x)$, and the asymptotic feature depends on the value of $\xi$; that is, $\xi>\xi_c$ or $\xi<\xi_c$. |
The typical solutions lor outgoing (rans-Las( magnetosonic Lows are demonstrated in Figures laa. and Ibb. for both cases of£<£. and £>£. | The typical solutions for outgoing trans-fast magnetosonic flows are demonstrated in Figures \ref{fig:outflow}a a and \ref{fig:outflow}b b, for both cases of $\xi<\xi_c$ and $\xi>\xi_c$. |
The outflows can start Irom the plasma source Cr<1). and after passing through the Alfvénn point (A) and the fast magnetosonic point (F) thev reaches distant regions. | The outflows can start from the plasma source $x\ll 1$), and after passing through the Alfvénn point (A) and the fast magnetosonic point (F) they reaches distant regions. |
In the ease of£<£.. the flow reaches ο>>1 region with a linite Mach number. | In the case of $\xi<\xi_c$, the flow reaches $x\gg 1$ region with a finite Mach number. |
This is the standard picture discussed by lots of previous wind mocels. | This is the standard picture discussed by lots of previous wind models. |
On (he other hand. in the case of£>€, the flow confines within. «rc. | On the other hand, in the case of $\xi>\xi_c$ the flow confines within $x<x_c$. |
We can expect (hat asvinplolically the magnetic field line becomes cvlindrical ancl (he flow streams towiid Z- | We can expect that asymptotically the magnetic field line becomes cylindrical and the flow streams toward $Z$ -direction. |
In the distant. Z-region (ζω>> 1). the flow becomes to have a very high. Alfvénn Alach number. | In the distant $Z$ -region $Z\Omega_F\gg 1$ ), the flow becomes to have a very high Alfvénn Mach number. |
Though we have constructed the basic formulae for discussing the evolution of M7. in (his paper we are particularly interested in highlv relativistic acceleration of bulk motion through a conversion of magnetic to kinetic energv. | Though we have constructed the basic formulae for discussing the evolution of $M^{2}$, in this paper we are particularly interested in highly relativistic acceleration of bulk motion through a conversion of magnetic to kinetic energy. |
In a sub-Allvénnic region the outflows are expected to be injected under a magnetic-energv dominated state (£7 LO) with a very large value of E. | In a sub-Alfvénnic region the outflows are expected to be injected under a magnetic-energy dominated state $E\simeq L\Omega_{F}$ ) with a very large value of $E$. |
This means that we can analvze the evolution of M? in more details. using the approximations For example. equation (23)) claims that the value of? at the fast-magnetosonie point becomes very large and is approximately given by £73 fj. in which the exact form of f=fCr) is necessarv because €=£(ry) may be very close to unity. | This means that we can analyze the evolution of $M^{2}$ in more details, using the approximations For example, equation \ref{position}) ) claims that the value of $x^{2}_{\rm F}$ at the fast-magnetosonic point becomes very large and is approximately given by $E^{2/3}f_{\rm F}$ , in which the exact form of $f=f(x)$ is necessary because $\xi_{\rm F} \equiv \xi (x_{\rm F})$ may be very close to unity. |
Hence. we can write the position | Hence, we can write the position |
innermosst region of NGO Figure4258 as observed with the SB2 imagefibre bundle of INTEGRAL. | st region of NGC 4258 as observed with the SB2 fibre bundle of INTEGRAL. |
The circle on the upper right marks the defective fibre a synthetic F658N image from our data by integrating the spectra with the wavelengths weighted with the transmission curve of that filter. | The circle on the upper right marks the defective fibre a synthetic F658N image from our data by integrating the spectra with the wavelengths weighted with the transmission curve of that filter. |
The image and contours show the above-mentioned strong absorption to the SW of the nucleus. | The image and contours show the above-mentioned strong absorption to the SW of the nucleus. |
In the (continuum-free) Ha image from the SB2 (with higher spatial resolution), the northern first detected by Ceciletal.(2000) stands out even more clearly than in images from the HST (see Fig. 2)). | In the (continuum-free) $\mathrm H\alpha$ image from the SB2 (with higher spatial resolution), the northern first detected by \cite{ceciletal00} stands out even more clearly than in images from the HST (see Fig. \ref{ha_sb2}) ). |
In our continuum-free Ha image, the contrast between the E and W sides of the loop seems weaker than in Ceciletal.(2000). | In our continuum-free $\mathrm H\alpha$ image, the contrast between the E and W sides of the loop seems weaker than in \cite{ceciletal00}. |
. 'There is even a hint of a southern counterpart of this loop in the asymmetric morphology below the nucleus, although severe obscuration by dust in this region makes it impossible to confirm. | There is even a hint of a southern counterpart of this loop in the asymmetric morphology below the nucleus, although severe obscuration by dust in this region makes it impossible to confirm. |
The nature of the loop(s) remains unclear. | The nature of the loop(s) remains unclear. |
A possible origin is that they are gas bubbles originating from the interaction of the jet with the dense ISM, as proposed by Ceciletal.(1992). | A possible origin is that they are gas bubbles originating from the interaction of the jet with the dense ISM, as proposed by \cite{ceciletal92}. |
. The velocity structure of the ionized gas, showing an asymmetry roughly along the N-S line, supports a connection with the jet. | The velocity structure of the ionized gas, showing an asymmetry roughly along the N–S line, supports a connection with the jet. |
On the other hand, the line ratios at those locations are not indicative of shocks. | On the other hand, the line ratios at those locations are not indicative of shocks. |
Thus, the possibility of the loop(s) being the edges of an ionization cone, as proposed in is also very attractive. | Thus, the possibility of the loop(s) being the edges of an ionization cone, as proposed in \cite{ceciletal00} is also very attractive. |
The velocity field in Fig. | The velocity field in Fig. |
3 shows the rotation pattern of the stars. | \ref{velstars}
shows the rotation pattern of the stars. |
A big area in the SW part of the FOV has been masked because the low S/N in the spectra induced by the high extinction in this region does not allow us to calculate a reliable velocity. | A big area in the SW part of the FOV has been masked because the low S/N in the spectra induced by the high extinction in this region does not allow us to calculate a reliable velocity. |
Even for the SB3 bundle, the FOV is quite small, and the velocity field of the ionized gas is too distorted to calculate a rotation model for the disc. | Even for the SB3 bundle, the FOV is quite small, and the velocity field of the ionized gas is too distorted to calculate a rotation model for the disc. |
We will therefore use the velocity field for the stars to subtract the rotating pattern of the galaxy from the gas components in order to generate residual velocity fields. | We will therefore use the velocity field for the stars to subtract the rotating pattern of the galaxy from the gas components in order to generate residual velocity fields. |
Obviously, there will be differences between the rotating pattern of the stars and the gas (namely the asymmetric drift). | Obviously, there will be differences between the rotating pattern of the stars and the gas (namely the asymmetric drift). |
We do expect these differences to be small enough for our purposes and, in any case, we will be very cautious when interpreting the residual velocity fields. | We do expect these differences to be small enough for our purposes and, in any case, we will be very cautious when interpreting the residual velocity fields. |
In this section we address the distribution and kinematics of the interstellar neutral gas. | In this section we address the distribution and kinematics of the interstellar neutral gas. |
In Fig. | In Fig. |
4 we present the distribution of the neutral gas detected by means of the equivalent width of the NaD doublet. | \ref{ewnad} we present the distribution of the neutral gas detected by means of the equivalent width of the NaD doublet. |
In Fig. | In Fig. |
5 we show the residual velocities obtained by subtracting the stellar velocity map from the NaD velocity map. | \ref{velnamstars} we show the residual velocities obtained by subtracting the stellar velocity map from the NaD velocity map. |
In the map of the equivalent width we can see a strip parallel to the major geometrical axis of the disc starting at the nucleus and extending some 15 arcsec to each side of the nucleus. | In the map of the equivalent width we can see a strip parallel to the major geometrical axis of the disc starting at the nucleus and extending some 15 arcsec to each side of the nucleus. |
This strip nicely traces the neutral gas of the near side of the galaxy that is absorbing the light coming from the stellar disc. | This strip nicely traces the neutral gas of the near side of the galaxy that is absorbing the light coming from the stellar disc. |
Of course, this is not all the neutral gas, but only the one that can be detected in absorption (we cannot see the neutral gas on the far side of the galaxy, nor can we see the neutral gas in the more extinguished region on the nearest side for the same reason). | Of course, this is not all the neutral gas, but only the one that can be detected in absorption (we cannot see the neutral gas on the far side of the galaxy, nor can we see the neutral gas in the more extinguished region on the nearest side for the same reason). |
Even with this obvious limitation, the detected distribution of cold neutral gas roughly resembles the distribution of molecular gas as seen in CO observations citeSawadasatohetal07)). | Even with this obvious limitation, the detected distribution of cold neutral gas roughly resembles the distribution of molecular gas as seen in CO observations \\cite{Sawadasatohetal07}) ). |
Figure ὅ shows the velocity of the neutral gas with respect to the underlying disc obtained by subtracting the stellar velocity map from the velocity map of the neutral gas. | Figure \ref{velnamstars} shows the velocity of the neutral gas with respect to the underlying disc obtained by subtracting the stellar velocity map from the velocity map of the neutral gas. |
Again, the morphology of the map resembles the residual maps obtained from CO observations by Sawada-Satohetal. (2007),, but in our case the residual velocities are much higher. | Again, the morphology of the map resembles the residual maps obtained from CO observations by \cite{Sawadasatohetal07}, but in our case the residual velocities are much higher. |
The detected neutral gas has huge residual velocities in the —120 to —370 km/s range with respect to the stellar disc. | The detected neutral gas has huge residual velocities in the $-120$ to $-370$ km/s range with respect to the stellar disc. |
Although Sawada-Satohetal.(2007) have proposed a warped disc with expansion to explain their data, we favour an alternative scenario to explain our detected morphology and kinematics of the neutral gas. | Although \cite{Sawadasatohetal07} have proposed a warped disc with expansion to explain their data, we favour an alternative scenario to explain our detected morphology and kinematics of the neutral gas. |
In our opinion our data seem to indicate that the detected neutral gas (which is on the near side of the galaxy) it is most probably moving radially outwards from the galaxy centre. | In our opinion our data seem to indicate that the detected neutral gas (which is on the near side of the galaxy) it is most probably moving radially outwards from the galaxy centre. |
We will elaborate a bit more on this scenario later on. | We will elaborate a bit more on this scenario later on. |
i0tometric uncertainty is adequate for this study that identifies "normal galaxy candidates on the basis of the ow X-ravtooptical Lux ratio logfx/fii | photometric uncertainty is adequate for this study that identifies `normal' galaxy candidates on the basis of the low X-ray–to–optical flux ratio $\log f_X / f_{opt} < -2$. |
This is estimated from the kkeV. Lux fx(0.5.—2keV) and the USNO-A2.0 B-band magnitude according to the relation The equation above is derived. from. the X-raytooptical [lux ratio definition. of Stocke et al. ( | This is estimated from the keV flux $f_X ( \rm 0.5 - 2 \,
keV)$ and the USNO-A2.0 $B$ -band magnitude according to the relation The equation above is derived from the X-ray--to--optical flux ratio definition of Stocke et al. ( |
1991). that involved kkeV. Dux. and. Y-band. magnitude. | 1991) that involved keV flux and $V$ -band magnitude. |
These quantities are. converted. to 0.5-2kkeV. Lux ancl -band magnitude assuming a mean colour BVLs nnand a power-law N-rav spectral energy. distribution with ΕΞ1.5. | These quantities are converted to keV flux and $B$ -band magnitude assuming a mean colour $B-V=0.8$ and a power-law X-ray spectral energy distribution with index $\Gamma=1.8$. |
The logfx/fap=2 cutoff although minimises the ACN contamination mav exclude from the sample X-ray. ultra-Iuminous galaxies such as powerful starbursts (c.g. 33256;" ...222107I: Moran. Lehnert Lelf 1999) or very massive ellipticals (Lx sts eg O'Sullivan. Forbes Ponman 2001). | The $\log f_X / f_{opt} = -2$ cutoff although minimises the AGN contamination may exclude from the sample X-ray ultra-luminous normal galaxies such as powerful starbursts (e.g. 3256; $\approx 2\times10^{42}$; Moran, Lehnert Helfand 1999) or very massive ellipticals $L_X>10^{42}$ ; e.g. O'Sullivan, Forbes Ponman 2001). |
Ceorgantopoulos et al. ( | Georgantopoulos et al. ( |
2005) argue that in the case of star-forming galaxies the logfy/fap,=2 limit is not likely to be a major source of incompleteness. at least for the 2 Universe. | 2005) argue that in the case of star-forming galaxies the $\log f_X /
f_{opt} = -2$ limit is not likely to be a major source of incompleteness, at least for the $z$ Universe. |
For carly tvpe galaxies we use the local 12/80 sample of Fabbiano et al. ( | For early type galaxies we use the local E/S0 sample of Fabbiano et al. ( |
1992) to estimate incompleteness because of the logfx/fi,=2 cutoll | 1992) to estimate incompleteness because of the $\log f_X / f_{opt} = -2$ cutoff. |
We find that about 20 per cent of the galaxies in that sample have logLx/Lg> 2. most of which are also luminous with Ly2107eres | We find that about 20 per cent of the galaxies in that sample have $\log L_X /L_B >-2$ , most of which are also luminous with $L_X
\ga 10^{42} \rm \, erg \, s^{-1}$. |
We note however. that some AGN contamination Is expected within this X-ray bright subsample. | We note however, that some AGN contamination is expected within this X-ray bright subsample. |
The logfxως2 regime is also. populated with Galactic stars. | The $\log f_X / f_{opt} < -2$ regime is also populated with Galactic stars. |
Phe USNO A2.0 catalogue does not discriminate between optically extended: and point-like sources. | The USNO A2.0 catalogue does not discriminate between optically extended and point-like sources. |
For this purpose we use the APM scans of the VAST that provide star/galaxy separation. | For this purpose we use the APM scans of the UKST that provide star/galaxy separation. |
We further quantify the reliability of the ADM star/galaxy classification below. using follow-up spectroscopic observations or CCD quality data from the 3rd release of the Sloan Digital Sky Survey (SDSS DIU). where available. | We further quantify the reliability of the APM star/galaxy classification below, using follow-up spectroscopic observations or CCD quality data from the 3rd release of the Sloan Digital Sky Survey (SDSS DR3), where available. |
A total of 102 sources in our NNMM saniple have logfxfas7 | A total of 102 sources in our XMM sample have $\log f_X / f_{opt} <
-2$. |
APM classifies 69 of them point-like and 30 extended (c.g. galaxies) with the remaining 3 having ambiguous classification. | APM classifies 69 of them point-like and 30 extended (e.g. galaxies) with the remaining 3 having ambiguous classification. |
The latter class is for objects that are assigned dillerent. ἵνρος on the red. and. blue UINST survey. plates. | The latter class is for objects that are assigned different types on the red and blue UKST survey plates. |
A total of 21 out of 102 sources in our NNMÁM sample with logfx/f.i2 have been observed. 5 of them are unresolved in APAL with the remaining 16 classified ealaxy-like. | A total of 21 out of 102 sources in our XMM sample with $\log f_X /
f_{opt} < -2$ have been observed, 5 of them are unresolved in APM with the remaining 16 classified galaxy-like. |
“Phe 5 point-like sources are included: in the targe list for follow-up spectroscopic observations to explore the reliability of the APM star/galaxy separation. | The 5 point-like sources are included in the target list for follow-up spectroscopic observations to explore the reliability of the APM star/galaxy separation. |
Low resolution optical spectroscopy was carried. ou with the Mexican 2-m class telescopes of the Observatorio Astrofisico. Guillermo. Haro. COAGLI) in. Cananea anc Observatorio Astronomico Nacional de San Pedro Martir (OAN SPAD. | Low resolution optical spectroscopy was carried out with the Mexican 2-m class telescopes of the Observatorio Astrofisico Guillermo Haro (OAGH) in Cananea and Observatorio Astronomico Nacional de San Pedro Martir (OAN SPM). |
Observations with the 2.d-m ΟΛΟΙ telescope were carried. out with the Boller Chivens (D&CCh) spectrograph and Lanclessternwarte Faint Objec Spectrograph and Camera (LFOSC) Zickeral et al. ( | Observations with the 2.1-m OAGH telescope were carried out with the Boller Chivens Ch) spectrograph and Landessternwarte Faint Object Spectrograph and Camera (LFOSC) Zickgraf et al. ( |
199 | 1997). |
The D&CCh spectrograph uses a Tektronix PAlo24AB CCD mounted at the Cassegrain focus giving a pixel scale of approximately aaresec. | The Ch spectrograph uses a Tektronix TK1024AB CCD mounted at the Cassegrain focus giving a pixel scale of approximately arcsec. |
We use a aaresec wide slit and a grating with 150llines/mam. providing a dispersion of A3.5Xpixel.+ and a wavelength MEN of =IDA (x ppixels EFAWHIAL) over the rangeAA. | We use a arcsec wide slit and a grating with lines/mm providing a dispersion of $\rm 3.5\,\AA\,pixel^{-1}$ and a wavelength resolution of $\approx \rm 15\,\AA$ $\simeq
4$ pixels FWHM) over the range. |
. The LEOSC is attached to the ο focus and is equipped with an EEV Ps603 385x578 CCL) giving a lO0xGaarcmün? feld of view and an image scale of Laaresee. | The LFOSC is attached to the Cassegrain focus and is equipped with an EEV P8603 385x578 CCD giving a $^2$ field of view and an image scale of arcsec. |
We used a 3aaresee wide slit and the G3 erism giving a wavelength resolution of zISA in the rangeAA. | We used a arcsec wide slit and the G3 grism giving a wavelength resolution of $\approx \rm 18\,\AA$ in the range. |
‘The observations were carried. out. during various observing runs between December 2003 and. March 2005. | The observations were carried out during various observing runs between December 2003 and March 2005. |
The observations with the 2.1-m OXN-SPM telescope were carried. out with the B&CCh spectrograph equipped with ΟΕΤο (1024x1024 pix) CCD installed at the Casscerain focus gi\‘ing a pixel scale of approximately aaresee. | The observations with the 2.1-m OAN-SPM telescope were carried out with the Ch spectrograph equipped with SITe3 (1024x1024 pix) CCD installed at the Cassegrain focus giving a pixel scale of approximately arcsec. |
We use a 22.5 areseewide slit and a erating with 300 linesfmm. providing a dispersion of AA//pix and an ellective instrumental spectral resolution of about | We use a 2.5 arcsecwide slit and a grating with 300 lines/mm, providing a dispersion of /pix and an effective instrumental spectral resolution of about |
variable background emission hinders any detection of such a pattern in andAIA-304À. | variable background emission hinders any detection of such a pattern in and. |
. When the bright streak in reaches the footpoint, a noticeable propagation in is initiated from the footpoint. | When the bright streak in reaches the footpoint, a noticeable propagation in is initiated from the footpoint. |
The dashed lines in plot mark the distinct events that occur right after the downflow event. | The dashed lines in plot mark the distinct events that occur right after the downflow event. |
The magnitude of the outward velocities vary from 57 km s! to 88 km s! | The magnitude of the outward velocities vary from 57 km $^{-1}$ to 88 km $^{-1}$. |
The outward streaks show pattern of about 10 minutes. | The outward streaks show quasi-periodic pattern of about 10 minutes. |
. Apparent downflows are frequently observed in a time sequence at temperatures lower than 1 MK. | Apparent downflows are frequently observed in a time sequence at temperatures lower than 1 MK. |
The two righthand panels in Fig. | The two righthand panels in Fig. |
1. show the temporal variations of ,and between 13:15 UTC and 13:25 UTC, at the beginning of a falling event. | \ref{fig_limb} show the temporal variations of and between 13:15 UTC and 13:25 UTC, at the beginning of a falling event. |
A brightening in and a darkening in the are simultaneously detected at the cross signs andB. | A brightening in and a darkening in the are simultaneously detected at the cross signs and. |
Figure 4 presents a time distance plot, where the two upper panels of Fig. | Figure \ref{fig_slice} presents a time distance plot, where the two upper panels of Fig. |
4 display original radiance in ,and171A,, while the bottom panel shows a temporal variation of to enhance small variations. | \ref{fig_slice}
display original radiance in and, while the bottom panel shows a temporal variation of to enhance small variations. |
The brightening in began at 13:40 UTC around a height of 80 Mm. | The brightening in began at 13:40 UTC around a height of 80 Mm. |
Small blobs in are seen to fall at a speed of 51 km s! starting 14:15 UTC. | Small blobs in are seen to fall at a speed of 51 km $^{-1}$ starting 14:15 UTC. |
A bright streak in appears at around 13:40 UTC and moves down slowly until 14:40 UTC when it starts falling at a speed of 65 km s!, following the cooler falling material seen inAIA-304A. | A bright streak in appears at around 13:40 UTC and moves down slowly until 14:40 UTC when it starts falling at a speed of 65 km $^{-1}$, following the cooler falling material seen in. |
. Just as the cool material reaches the surface, a noticeable upward motion at a speed of 82 km s! in is initiated. | Just as the cool material reaches the surface, a noticeable upward motion at a speed of 82 km $^{-1}$ in is initiated. |
Similarly, in Fig. 3,, | Similarly, in Fig. \ref{fig_slice_m}, |
an outward motion in is induced immediately following the inward motion in171À. | an outward motion in is induced immediately following the inward motion in. |
. The results indicate that the hot upflowing pattern is enhanced after cool downflowing events. | The results indicate that the hot upflowing pattern is enhanced after cool downflowing events. |
Figure 5 displays normalized lightcurves integrated over the 5x5" box surrounding in Fig 1.. | Figure \ref{fig_lc2} displays normalized lightcurves integrated over the $\times$ box surrounding in Fig \ref{fig_limb}. |
The radiance at 17:30 UTC is subtracted from the measured radiance to compensate for the background. | The radiance at 17:30 UTC is subtracted from the measured radiance to compensate for the background. |
The assumption of a constant background is reasonable, since the pre-event radiance at 12:00 UTC and the postevent radiance at 17:30 UTC were quite similar. | The assumption of a constant background is reasonable, since the pre-event radiance at 12:00 UTC and the postevent radiance at 17:30 UTC were quite similar. |
Shows a broad peak with a small dip at 13:30 UTC, when ,and rapidly increased. | shows a broad peak with a small dip at 13:30 UTC, when and rapidly increased. |
This emission variation is interpreted as the cooling of plasma. | This emission variation is interpreted as the cooling of plasma. |
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