Broad line radio galaxies (BLRGs) are rare kind of AGNs where the emission from the accretion disc is visible as well as the extended jet emission. Direct comparison of broad-band spectrum in BLRGs to those of Sy-1s provides important clue to understand the formation of relativistic jets. We propose a 160 ksec (40ksec x4) observations of the brightest BLRG 3C120 with Suzaku. Recent XMM and Beppo-SAX observations confirm remarkable spectral features including fluorescent Fe line. Our goals are three folds; (1) Monitoring the variability correlation between Fe line and the Compton reflection hump, (2) Precise measurement of total luminosity as a probe of various accretion states, and (3) Resolving excess soft components, warm absorber, and 6.9 keV line, which are still under debate.

We have a new idea that a magnetized white dwarf can be a particle-acceleration cite to emit non thermal emission. In order to understand the particle acceleration process in rotation-powered objects, it is important to measure the hard X-ray emission from magnetized white dwarfs, in addition to that from well-known neutron stars. Here, we propose a 100ksec observation of a magnetic cataclysmic valiable, AE Aqurii. It is difficult for INTEGRAL mission, and is challenging even for the HXD, but it will be a ``first detection'' of the non-thermal emission in the hard X-ray band from a white dwarf with Suzaku.

We request a 100ks Suzaku observation of the bright Seyfert galaxy, MCG -5-23-16 simultaneously with approved XMM-Newton and Chandra HETG observations in December 2005. MCG -5-23-16 has one of the best known examples of a relativistically broadened iron K line. With a Swift-BAT flux of 1.6e-10 cgs (15-100 keV), it is one of the brightest AGN above 10 keV. The simultaneous observations will allow us to determine the shape of the broad relativistic Fe line after subtracting the narrow line components measured by HETG. Importantly, Suzaku's wide bandpass will accurately measure the broad-band continuum and reflection component of MCG -5-23-16, essential for constraining the broad iron line. These observations will also allow us to determine the temperature of the high energy cut-off.

(i) Early break in lightcurve of X-ray afterglows using HXD. Recent Swift/XRT observations reveal that early X-ray afterglows of GRB has flat portion with very shallow decay. It may suggest continuous energy input from the central engine. The transition from its phase to general afterglow may display hard-to-soft evolution reflecting the cooling frequency. Thus multi wavelength observation will provide a key to the physics of central engine activity. (ii) Emission lines in the afterglows. The confirmation of line existence should be a matter of great importance because there remains unanswered questions. Some data may indicate a prominent iron line but others seem to suggest significant lower energy lines instead without iron lines.

No cluster has had its X-ray temperature measured out to the virial radius. Hence no cluster has had it total mass measured using X-ray methods. Typically these measurements extend only to 60% of the virial radius. We propose to perform these measurements for the first time and with high accuracy for the relaxed cluster A1413. The low Suzaku background permits us to make this measurement.

We propose to obtain a broad band spectrum of the narrow-line Seyfert 1 (NLS1) NGC 4051. NLS1s are often presumed that they host a relatively small black hole with a very high accretion rate. Such a class would have played an important role in the growth of black holes in a cosmological context. We will measure the intrinsic photon index, amount of reflection, and high energy cutoff for the first time to investigate an accretion disk under a high accretion rate and compare them with conventional broad-line Seyferts.

NGC 2992 is a nearby Seyfert 1.9 galaxy showing long-term (20 yrs) large amplitude (factor of 20) variability. This object showed switching between Compton-thick and -thin. Recent RXTE monitoring has shown that this object is highly variable on shorter time scales (2 weeks). We propose three Suzaku observations to monitor the variability of absorption column, broad band continuum shape, and Fe line intensity to understand the cause of the remarkable variability.

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The center of the Fornax cluster was observed with Suzaku with a 80 ks exposure. We have detected excess hard-emission and derived O abundances of the ISM of NGC 1399 and NGC 1404, and the intracluster medium (ICM). Here, we propose to observe two offset pointings of the Fornax cluster for 160 ks (80 ks times 2) to study the distribution of the hard emission and the abundance distribution of O, Mg, Si, S and Fe.

The supernova remnants (SNRs) are most convincing candidates for the acceleration of cosmic-rays. Together with the TeV gamma-ray detection by CANGAROO and HESS, it is now confirmed that at least some of the SNRs can actually accelerate electrons up to > 10 TeV. However, such studies have not provided direct information on ``protons'', which is the major component of cosmic-rays. Here we propose to measure spatial distribution of accelerated protons in the shell of RCW 86, and its association with the high energy (>10 TeV) electrons which emit synchrotron X-rays up to 50 keV. Large effective area and the good detection capability of Suzaku will be ideal tools for our scientific goal.

We propose to obtain high quality spectrum near the GC. The objective is to resolve 6.4, 6.7, and 6.9 keV line and determine the high energy tail and sub-structures, which may be X-ray reflection from Sgr A* (6.4 keV line + 7.1 keV edge + high energy tail), thermal plasma (6.7 + 6.9 keV lines, with no hard X-ray tail), non thermal emission (e.g. line but hard X-ray tail). Unexpected spectral feature could be also found, depending on the real origin.

A1060 is a bright non cD cluster and gives us a unique opportunity to study injection process of metals in the intracluster space. Reliable measurement of oxygen distribution with XIS will tell us whether the metals produced by Type-II supernova (mainly oxygen) ditributes over a different scale compared with the SN-Ia product (Fe). A1060 is the best cluster where we can directly observe distribution of metals produced by general cluster galaxies. Also, central increase of temperature by 20%, probably connected with motions of bright central galaxies, suggests that non-thermal X-rays may be produced.

We propose a 100 ksec Suzaku observation of the Galactic microquasar V4641 Sgr in an outburst. V4641 Sgr has many unique charactersitics:1)giant X-ray outbursts with fast rise and decay times, 2)violent variability in the X-ray and optical bands, and 3)remarkable iron-K disk-line profiles in the X-ray spectrum. However, it is hardly understood due to the poor X-ray coverage which is partly the result of the short outburst duration and rapid intensity variations of this source. Hence, we collaborate closely with VSNET and RXTE/ASM team for the rapid trigger. The moderate energy resolution and wideband energy coverage of Suzaku enable us to clarify the radiation mechanisms of V4641 Sgr. This observation is now planed simultaneously with RXTE and many optical-near IR observatories.

We propose to observe the central region of the Sculptor supercluster at z=0.11, in a search for the theoretically predicted Warm/Hot Intergalactic Medium (WHIM). The WHIM has been 'missing' observationally, until recent detection of the X-ray absorption due to the ionized light elements in the background quasar spectra. Still there is no confident detection of the expected soft X-ray emission. This is mainly because that the X-ray brightness is very low, compared to the Galactic diffuse emission in the soft X-ray band and/or the spectral sensitivity of previous experiments are limited. To separate the expected X-ray lines of the WHIM (mainly O VII) from the Galactic emission, we select an unique supercluster at z>0.1.

We propose Suzaku observations of two luminous low-mass X-ray binaries (Z sources), GX 349+2 and Cyg X-2, to investigate the origin of the hard tails of Z sources, of which the spectral photon indices are reported to become occasionally less than unity. With the high sensitivity of the HXD, we detect the spectral shape up to several 100 keV and reveal existence of particle acceleration caused by high radiation pressure.

SN1987A is providing us with a unique opportunity to study the supernova explosion itself and the very early phase of the supernova-remnants evolution. The supernova blast wave has started to strike the inner circumstellar ring. The neutrino flash observed at the time of explosion implies the formation of a neutron star, but no evidence of this has been detected yet. We propose to observe SN1987A for 40 ksec with Suzaku HXD and XIS. Our first goal is the search for a periodic hard signal from the putative pulsar. We also want to study the collision of the supernova blast wave with the inner ring. In order to follow the temporal evolution of the shock, we propose to observe the source with Suzaku in the early phase of the SWG PV-phase as a reference for further studies.

HESS found several new TeV sources in the Galactic Plane Survey. Possible origin would be PWN or synchrotron X-ray SNR shell. However many of these new TeV sources (their sizes are ~10 arcmin) have no counterpart in any other wavelength. They can be main contributors to the Galactic Cosmic rays. In order to reveal the nature of these fantastic objects, we propose to observe the extended sources. HESS~J1616-508 is already observed and we found this source has quite low surface brightness in X-rays compared with TeV gamma-rays, indicating this is a dark particle accelerator Here, we point out HESS~J1804-216 which has possible counterparts in other wavelengths, then it might be the missing link between known Galactic accelerators and dark particle accelerators.

We propose to observe an isolated elliptical galaxy NGC720 with Suzaku. Isolated elliptical galaxies are important to probe the ISM metal abundance, since their hot gas is not affected by the amibient bright intracluster medium which often exists around X-ray bright elliptical galaxies. Suzaku is expected to measure the Oxygen abundance in the ISM bettern than XMM-Newton and constrain the origin of metals in the ISM and also ICM. Dark matter content around elliptical galaxies can also be constrained better than XMM-Newton. Such a measurement is difficult for X-ray bright galaxies due to the superposition of the cluster potential.

We propose a 100 ks observation of the nearest ultraluminous infrared galaxy (ULIG) Arp220. The major objective is to search for evidence of heavily obscured nuclei. First detection of a Compton-thick source may be possible with the HXD's sensitivity, if a powerful nucleus is present, leading to a major discovery. The good quality XIS spectrum can be decisive for the origin of the strong Fe K line, barely detected with the previous XMM-Newton observation.

The broad iron line in the Seyfert 1 galaxy MCG-6-30-15 shows that most of the power is released at 2--4 gravitational radii enabling the strong gravity, accretion flow and energy release in that exciting regime to be studied. The spectral variability of the source decomposes into a highly variable power law and a reflection-dominated component, containing the iron line and Compton hump, which varies significantly but with much less amplitude. This can be explained by the extreme gravitational light bending occuring in this region. We propose to observe MCG--6-30-15 for 4 x 50~ks in order to determine for the first time the variability of the reflection over a wide range of energies from below 1 keV to above 40 keV and timescales .

A426 is the X-ray brightest cluster in the Sky. The core is X-ray peaked, has a short radiative cooling time, a temperature drop and a central radio source which is blowing bubbles in the intracluster medium. A radio minihalo extends over the central 6 arcmin. A coincident power-law component is seen in deep Chandra data. This is likely to be inverse Compton emission from the electron population responsible for the radio emission. The region is expected to be a luminous, extended, hard X-ray source easily detectable by the Suzaku HXD. Confirmation of this hard X-ray component will enable the magnetic field to be securely determined in the intracluster gas.

To study populations of non-thermal and hot thermal electrons, we propose TOO observations of two black hole binaries (BHBs), XTE J1550-564 and GROJ1655-40, in the very high state (VHS). These two sources are well studied BHBs, and their VHS can be clearly distinguished based on the RXTE/ASM. Though origin of non-thermal hard X-ray emission which is generally observed in high accreting BHBs has long been a great mystery for black hole physics, in the VHS, the location of at least the hot-thermal electrons has been found to exist closely to the optically thick accretion disk like disk corona. By the good spectra at 50-500keV with the HXD, we can distinguish whether the non-thermal electrons have same population as the hot-thermal electrons or not.

We propose a 150 ks observation of the giant radio relic in the west of the A3376 cluster. A3376 is a low temperature (4.5 keV) cluster with possible excess hard X-ray emission in 2.7 sigma significance by Beppo-SAX, and also with a pair of giant radio relics. This target is best suited for cluster hard excess survey with HXD. Following the first observation planned around October 2005 located near the east relic, the observation of the west relic 23 arcmin away can bring us the first spacial information on cluster excess hard X-rays.

We propose a 100 ks observation of the NLS1 1H 0707--495 in order to understand its remarkable and puzzling spectral and variability properties. The Suzaku data will help us to disentangle between the two interpretations adopted so far, namely partial covering and relativistically blurred reflection.

A 100ks Suzaku observation of the NLS1, PG 1211+143 is proposed. Previous XMM-Newton and Chandra observation claimed both blue-shifted (0.1c) and redshifted (0.26c-0.40c) iron Kalpha absorption lines. The redshifted iron K lines may originate from matter falling onto the supermassive black hole. The high effective area and low background of Suzaku XIS above 5 keV will enable us to measure these relativistically shifted iron lines in PG 1211+143 with great accuracy. Constraining the time variability of the lines will allow us to determine the physical origins of the absorption, e.g. failed jet/outflow or gravitational redshift from a Kerr black hole. The excellent broadband capabilities of Suzaku will accurately determine the continuum, essential for modeling the iron K band.

We propose to observe the blank Galactic plane field at (l,b)=(28.6,0.0) for 200 ksec to study energy spectra of Galactic Ridge X-ray Emission. This is a Chandra deep field where we have spent 100 ksec. We will carry out plasma diagnostics of the Galactic ridge emission using primarily iron lines, and also Kalpha and Kbeta lines of Ne, Mg, Si, and S. The 200 ksec Ridge observation by Suzaku enables us to compare Galactic center and ridge emission lines directly. We believe the Galactic Ridge X-ray emission is truely diffuse, based on our Chandra study. However, there is a claim that the ridge emission is preimaly composed of dim sources down to 10^-16 cgs in 2-10 keV. To end the controversy, we plan to carry out a 1Msec Chandra observation on this Chandra-Suzaku field.

Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst.

Although the boundary layer that is formed between the rapidly rotating inner accretion disk and the white dwarf surface has been known as a hard-X-ray emitter, its geometry and structure has not been well understood yet. We aim to investigate the boundary layer structure with SS Cyg, the brightest dwarf nova, by means of a soft X-ray component with the BI CCD, a fluorescent Fe K-alpha line with the FI CCDs, and a continuum reflection by the white dwarf surface with the HXD PIN. It is of great use to observe states of a different mass accretion rate, and hence we propose to observe both in quiescence and in outburst.

We propose to observe two lobes of X-ray and gamma-ray emission from the shell remnant RXJ 0852-4622 (Vela Jr) with HXD. The 1-10 keV spectrum of this remnant is essentially a featureless continuum attributed to synchrotron emission from accelerated electrons, with the X-ray and gamma-ray morphologies being very well matched. Observations at energies above 10 keV with HXD will probe the cut-off energy of the synchrotron spectrum, shedding light on the electron acceleration efficiency. The large size of the remnant makes it possible to observe different portions of the limb with separate HXD PIN observations.

We propose to use Suzaku XIS to observe regions of diffuse emission in the Magellanic Clouds. The diffuse component was identified by ROSAT PSPC observations, but has never been studied with a true spectroscopic instrument. Suzaku is well-matched to the angular size and expected temperature of the regions of diffuse emission in the LMC. Not only will such observations give a clear view of the temperature structure of this gas, they will provide a direct measurement of ambient abundances in the Clouds.

Cometary X-ray emission is likely the result of charge exchange interactions between the highly charged solar wind and neutral material ablated from the nucleus. Recent measurements using Chandra coupled with precise laboratory measurements at EBIT lend support for this hypothesis. In fact we have successfully deconvolved the Chandra/ACIS observation of comet C/Linear using direct observations of charge exchanging plasmas at EBIT using a flight spare XRS detector system. Here, we propose to observe a magnitude 1 comet, 73P/SW 3, the brightest comet of the decade during May 2006 within only 0.08 AU of the earth using the XIS1 (BI) instrument on Suzaku. The exceptional low energy response of the XIS will allow us to unambiguously identify the x-ray emission mechanism in comets.

We propose a 120 ks Suzaku observation of Abell 1795. Five overlapping XIS pointings will: i) map the temperature to the virial radius for the first time; ii) check for the presence of soft excess emission and, if found, possibly determine whether the excess is associated with the cluster or our Galaxy; and iii) determine the run of abundance with radius in detail at r< 500. This observation will demonstrate the scientific value of the low-background and good spectral resolution of the Suzaku XIS in cluster studies.

We propose to obtain high-quality spectra of the X-ray brightest, compact group of galaxies HCG62 with Suzaku. The previous ASCA observation has reported that this group has a hard tail in the spectrum. With 100 ksec exposure, we can constrain the flux of the hard component above ~3 keV with much higher accuracy. This will give a great impact in understanding the origin of the hard emission and non-thermal populations in the IGM. Furhtermore determining the metal abundance, particularly Oxygen, in the central and outer regions will give us new, valuable information on metal enrichment processes in the group that is not dominated by a cD galaxy. Suzaku/XIS is the best-suited for our scientific objectives since it has a low background level and the unprecedented high sensitivity.

We propose to monitor a transient black hole binary in outburst through a series of 20 ks observations. Our goal is to map the physical conditions in the accretion disk as the source evolves through the various continuum states using the spectral diagnostics available in the Fe K fluorescence emission. Measurements of the Fe K emission will allow us to quantify the thermal, kinematic, and geometric conditions in both the disk and the surrounding material. Correlating the Fe K diagnostics with sensitive measurements of the direct and reprocessed continuum emission will allow us to map the evolving conditions and constrain models of the dynamic accretion processes in black hole binaries. We will monitor 7 targets with the RXTE. This observation will be triggered when one becomes active.

Suzaku can potentially determine the time since the nearby supernova that created (or reheated) the Local Hot Bubble (LHB) by measuring the ratio of the O VII/O VIII lines emitted by the LHB. The LHB temperature is ~10^6 K, and in equilibrium we would expect no O VIII emission. However, the LHB is almost certainly not in equilibrium, and it is quite possible that significant O^{+7} is still recombining (and emitting O VIII) following its creation in the most recent local supernova 2-4 Myr ago. We propose to measure these lines from the LHB using the nearby molecular cloud MBM12 as a curtain to shadow more distant emission. Even if O VIII is not detected, the O VII measurement will be the first unambiguous measurement of a line from the LHB.

We propose two 50 ks observations, one for each of two EGRET blazars, 1510-089 (OR -017) and 0836+710 (4C +71.07). Both objects show extremely hard X-ray spectra, with photon indices about 1.3. The blazar 1510-089 ($z = 0.361$) is among a few OVV quasars showing prominent soft X-ray excess. The blazar 0836+710 ($z = 2.172)$ is the brightest X-ray source among the high redshift ($z>2$) quasars, and its very hard X-ray spectrum extends down to soft X-rays. Studying spectral shape and variability in the soft X-ray band relative to variability in the mid X-ray and optical bands can help to reveal nature of the soft X-ray excess of unknown origin, and multifrequency variability studies can provide constraints on the structure of jets on subparsec scales.

We propose two Suzaku pointings of the Galactic supernova remnant (SNR) that exploded as a supernova in 1006. The main goal of the project is to use the XIS measure the abundances of low-Z elements in the ejecta.

A dramatic central concentration of iron and silicon is present in the Centaurus cluster. Apart from this well-recognized contribution from Type Ia supernova, enrichment process due to Type II supernova is poorly understood. Centaurus cluster is most suited for the study of large-scale oxygen distribution, for which XIS is most sensitive. The XIS data will give us a key knowledge about how past Type II supernova have affected the enrichment process. The data would also confirm that the central gas is a mixture of hot and cool components with much better sensitivity than before.

Large-scale X-ray nebulae up to a few tens of kpc have been often found in starburst galaxies, which is thermally heated up by the superwind from the starburst nucleus. Iwasawa et al. (2003) found a large X-ray nebula up to 16kpc around NGC4388, which is photoiionized by Seyfert nucleus. Thus, this result suggests that the hard X-ray emission from active galactic nucleus could be a prime heat source of nebula. The goals of this observation are (1) to see how far the X-ray nebula is extended, (2) to obtain its precise X-ray spectrum, (3) to determine what is the X-ray emission mechanism, and (4) to exam if the photoionization by AGN could be a prime heat source of the galactic halo. We determine the photon index and the high energy cut-off of the power-law component from the HXD spectrum.

We propose 100 ksec observation of the Sgr C cloud in the Galactic center region. The cloud emits strong 6.4-keV line, and is a candidate of X-ray reflection nebula; the molecular cloud which emits fluorescence and scattered X-rays irradiated by an external X-ray source. The past activity of Sgr~A$^*$, the Galactic nucleus, may be the origin of 6.4-keV line. We will study 6.4-keV line and verify the X-ray reflection scenario. The second objective is to study the distribution of high ionized and neutral iron lines in the GC region. Chandra observation indicates that H-like iron line is very strong in this region. With the higher energy resolution of XIS, we can confirm the Chandra results. High energy diffuse emission above 10 keV is also a important target by HXD.

The X-ray spectrum of the 7 second LMXRB pulsar 4U1626-67 is dominated by low energy line emission with little evedence of iron K line in the pulse phase resolved spectra. It showd also cyclotron line at 37 keV that departs from the correlation of energy cutoff cyclotron energy observed in many other X-ray pulsars. This Suzaku observation allow to characterize the overall continuum, the low energy, the iron K alpha and cyclotron lines as function of the pulse phase,

CH Cygni is a symbiotic star in which a white dwarf is believed to be accreting the wind of the red giant. ASCA observation revealed a complex X-ray spectrum consisting of a heavily absorbed hard component and a relatively unabsorbed soft component. We propose to obtain the spectrum of CH Cyg above 10 keV for the first time using Suzaku HXD (PIN), while simultaneously obtaining high quality spectrum below 10 keV with the XIS.

We propose to observe NGC 4636 for 50~ksec in a single pointing, to determine the chemical evolution of elliptical galaxies via the determination of the spatially resolved abundance of Oxygen and other elements. Being one of the most X-ray luminous ellipticals, and having been observed by both Chandra and XMM, this is also an important target to compare the capabilities of the three observatories and interpret the results of the Suzaku XIS in light of the source spectrum provided by the XMM RGS.

Recently the BAT gamma-ray detector onboard Swift satellite has discovered very flat hard X-ray sources with photon index ~ 1.5 above 100 keV. The x-ray spectrum obtained with the XRT on Swiftis highly variable on time scales < 90 minutes. This variability and flat continuum spectrum suggests that this source is classified as a blazar. If this association is real, we have a precious chance to obtain spectrum upto several hundred keV in the source frame of the source. This wide range is of particularly importanceto study the blazar spectrum, or the electron distribution.

We propose four 20 ksec observations of the northeastern limb of the Cygnus Loop supernova remnant to study a recently discovered carbon rich region. This region seems to be the result of the interaction between the shock and an interstellar cloud or the cavity wall. Because of the superior spectral resolution and low background of the XIS in the low energy region, these pointings can also be used for the study of the C-N-O abundance ratio of the ISM in the vicinity of the Loop.

Simultaneous Observation of PKS2155-304 with XMM-Newton

To confirm the presence of redshifted oxygen lines from the WHIM surrounding A2218, we propose observations of 2 positions. One is a 35 ksec pointing on A2218 to raise the photon statistics of the oxygen feature, and the other is a 15 ksec pointing at about 1 degree west of the cluster to know the amplitude of the intensity variation of the Galactic oxygen lines.

We propose the calibration observations for XIS: E0102-72 ... Gain and QE in the low energy band Cas A ... Gain and QE in the high energy band Eta Carinae ... Contamination of the BI chip

We propose a 100 ks observation of LockmanHole with Suzaku. The main purpose is to obtain a template dataset of HXD background.

We propose to observe Tycho's Supernova Remnant with Suzaku. The proposal has two main goals: (1) to measure the energy spectrum of the entire remnant above 10 keV with the HXD, and (2) to study the 0.5-10 keV band spectrum as a function of position with the XIS.

Jets in blazars are believed to be a powerful site of particle acceleration. TeV emitting blazars are very important, because we can study very end of electron distribution near the maximum energy by using X-ray spectrum, because X-ray emission is believed to be due to synchrotron emission from the higher energy electron. Comparison of spectral index between X-ray and TeV gives us a crucial information on these source, because this is very sensitive to the particle injection and rapid cooling. In order to maximize the capability of sensitive hard X-ray observations of Suzaku, we propose reserved TOO observations for the next six months of PV phase from the TeV emitting blazars established by HESS, selected from five candidates.

We propose to observe NGC 2403, which is a nearby luminous normal spiral. Our main objective is to search and investigation of diffuse emission components. These include both rather soft (kT = 0.1 - 1 keV) ones already detected from a fair number of spirals, and hot (kT = a few keV) emission which, if established, may become an analogue to the Galactic ridge emission.