GHz Source Research Articles

On the Nature of the Hard X-Ray Source IGR J2018+4043

We found a very likely counterpart to the recently discovered hard X-ray source IGR J2018+4043 in the multi-wavelength observations of the source field. The source, originally discovered in the 20-40 keV band, is now confidently detected also in the 40-80 keV band, with a flux of (1.4 +/- 0.4) x 10(-11) erg cm(-2) s(-1). A 5 ks Swift observation of the IGR J2018+4043 field revealed a hard point-like source with the observed 0.5-10 keV flux of 3.4(+0.7)(-0.8) x 10(-12) erg cm(-2) s(-1) (90% confidence level) at alpha = 20h18m38.55s, delta = +40d41m00.4s (with a 4.2" uncertainty). The combined Swift-INTEGRAL spectrum can be described by an absorbed power-law model with photon index gamma = 1.3 +/- 0.2 and N_H = 6.1(+3.2)(-2.2) x 10(22) cm(-2). In archival optical and infrared data we found a slightly extended and highly absorbed object at the Swift source position. There is also an extended VLA 1.4 GHz source peaked at a beam-width distance from the optical and X-ray positions. The observed morphology and multiwavelength spectra of IGR J2018+4043 are consistent with those expected for an obscured accreting object, i.e. an AGN or a Galactic X-ray binary. The identification suggests possible connection of IGR J2018+4043 to the bright gamma-ray source GEV J2020+4023 (3EG J2020+4017) detected by COS B and CGRO EGRET in the gamma-Cygni SNR field.

CHIRAL MULTIPHOTON ABSORPTION AND INVERSE SKIN EFFECT IN WLAN SYSTEMS

A model formed by chiral bioplasma with a set of macromolecules of DNA, which represents the human head inner structure, makes possible to analyze its behavior, when it is radiated by a microwave electromagnetic field from cellular phones and WLAN’s at frequencies of 2.4 and 5.2 GHz is presented. The finite difference time domain, FDTD, numeric technique is used under multiphoton regime deduced from Maxwell equations. The numerical results of the Specific Absorption Rate, SAR, show the SAR behavior in function of input power and the chirality factor. The main conclusions of our work are: a) the microwave absorption from cellular phones or WLAN’s is enhanced, compared with classical models, when values of the normalized chiral factor are of order of one which appear under multiphoton regime ; b) a phenomena like an “inverse skin effect” in 5.2 GHz, with respect to a 2.4 GHz source, was observed. c) In the metamaterial region we show that the absorption rate always is positive.

Radio Observations of the Hubble Deep Field-South Region. II. The 1.4 GHz Catalog and Source Counts

This paper is part of a series describing the results from the Australia Telescope Hubble Deep Field–South (ATHDFS) survey obtained with the Australia Telescope Compact Array. This survey consists of observations at 1.4, 2.5, 5.2, and 8.7 GHz, all centered on the Hubble Deep Field–South. Here we present the first results from the extended observing campaign at 1.4 GHz. A total of 466 sources have been cataloged to a local sensitivity of 5 σ (11 μJy rms). A source extraction technique is developed that (1) successfully excludes spurious sources from the final source catalogs and (2) accounts for the nonuniform noise in our image. A source catalog is presented, and the general properties of the 1.4 GHz image are discussed. We also present source counts derived from our ATHDFS 1.4 GHz catalog. Particular attention is given to ensuring that the counts are corrected for survey incompleteness and systematic effects. Our counts are consistent with other surveys (e.g., the Australia Telescope ESO Slice Project, VIRMOS, and the Phoenix Deep Field), and we find, in common with these surveys, that the HDF-N counts are systematically lower.

Radio Identifications of Recently Discovered Planetary Nebulae

Using the 1.4 GHz NRAO VLA Sky Survey (NVSS) images and source catalog, we identified 315 radio sources stronger than ≈2.5 mJy among over 1000 recently discovered planetary nebulae north of J2000 declination δ = -40°. Two-thirds of these radio sources are weaker than 10 mJy at 1.4 GHz. This result is a uniform supplement to the previous NVSS radio identification of known PNe and a large homogeneous sample including over 1000 PNe with NVSS sources is obtained. By examining the radio properties of PNe, it is found that most of the planetary nebulae detected at both 1.4 and 5.0 GHz are optically thick at λ = 20 cm.

Close Association of an Extreme‐Ultraviolet Sunspot Plume with Depressions in the Sunspot Radio Emission

We obtained coordinated observations of the large sunspot in NOAA Region 8539 on 1999 May 9 and 13 with the Very Large Array and three instruments (CDS, EIT, MDI) aboard the Solar and Heliospheric Observatory satellite. The EUV observations reveal a plume in the sunspot umbra on both observing dates. The plume appears brightest in emission lines formed at temperatures between 1.6 × 105 and 5.0 × 105 K. Radio emission from the sunspot umbra is dominated by thermal gyroemission from the plume, which accounts for radio brightness temperatures <1 × 106 K in the umbra on both dates, as well as umbral brightness temperature depressions in the 4.535 and 8.065 GHz observations on May 13. A compact 14.665 GHz source persists near the umbra/penumbra boundary during our observing period, indicating a long-lived, compact flux tube with coronal magnetic field strength of at least 1748 G. It occurs in a portion of the sunspot that appears very dark in EUV emission.

12.2 GHz survey towards 6.7 GHz methanol masers

We present results of a 12.2 GHz methanol maser survey done with the Torun 32 m radio telescope. We examined 261 star forming-sites, known as containing 6.7 GHz maser emission sources. The survey resulted in 49 sources with maser line detection, with 21 previously unknown emissions. All detected 12.2 GHz masers have been observed at the 6.7 GHz transition. Only one 12.2 GHz source had no 6.7 GHz counterpart. We compared basic spectral line properties at both transitions. In a few cases we observed absorption features and emitting counterparts in the other monitored frequency, at the same velocity.

The Phoenix Deep Survey: The 1.4 GH[CLC]z[/CLC] Microjansky Catalog

The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg2, an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1 σ rms noise of 12 μJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 μJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 < z < 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The 1.4 GHz mosaic image and the source catalog are available on the World Wide Web; or from the authors by request.

Impact of Future Submillimeter and Millimeter Large Facilities on the Studies of Galaxy Formation and Evolution

ABSTRACTWe investigate what we can learn about galaxy formation and evolution from the data which will be obtained by the forthcoming large submillimeter/millimeter facilities, mainly by the Atacama Submillimeter Telescope Experiment (ASTE) and the Atacama Large Millimeter Array/Large Millimeter and Submillimeter Array (ALMA/LMSA). We first calculate the source counts from 350 μm to 3 mm using the empirical infrared galaxy number count model of Takeuchi et al. Based on the number counts, we evaluate the source confusion and determine the confusion limit at various wave bands as a function of the characteristic beam size. At submillimeter wavelengths, source confusion with the 10–15 m class facilities becomes severe at the 0.1–1 mJy level, and astrometry and flux measurements will be difficult. However, we show that a very large area survey of submillimeter sources brighter than 10–50 mJy can provide a unique constraint on infrared galaxy evolution at z = 1–2, and such a survey is suitable for the ASTE. In addition, such a survey enables us to study the clustering properties of submillimeter sources, which are still highly unknown. We also find that the 5 σ confusion limit of LMSA is fainter than 1 μJy, which enables us to study the contribution of sources at extremely large redshift. When we discuss such a deep flux limit, the dynamic range of a detector should be taken into account, since extremely bright sources make it impossible to detect the faintest sources near the detection limit. We evaluate the probability that sources that are 103 times brighter than the 5 σ detection limit of LMSA and ALMA exist in the field of view. We find that the probability is ≲3 × 10-4, and therefore we do not have to worry about the dynamic range. The source counts at such faint flux levels give important information about the epoch of galaxy formation. We then show that multiband photometry from the infrared (by ASTRO‐F) to the millimeter can be used as a redshift estimator. We examined the performance of this method by Monte Carlo simulations and found that it works successfully if we have reasonable measurement accuracy. In addition, we compare the observed 1.4, 5, and 8 GHz source counts with our model counts to examine the contribution of star‐forming galaxies to faint radio galaxies. We find that the faintest radio number counts (∼1 μJy) are dominated by actively star‐forming galaxies which lie at intermediate redshift z∼1–2.

A Complete Microjansky Radio Survey

The Phoenix Deep Survey is an ongoing multi-wavelength survey of a 2° diameter field aimed at studying the properties of the sub-mJy and μJy radio population. Here, we present the latest 1.4 GHz observations of this field. The new data, reaching a 5 σ flux level of 45 μJy at the centre of a 50′ diameter field, comprise more than 700 sources with flux densities less than 1 mJy (187 of which have S1.4 < 100 μJy). This provides one of the deepest radio (1.4 GHz) surveys currently available. The 1.4 GHz source counts are presented and show a flattening down to the 50 μJy level. At flux densities around 300 μJy there are indications that the sources detected may exhibit higher clustering than those observed at higher flux levels. This suggests that deep radio surveys could be useful for studies of large-scale structure but it also presents a warning for the representativity of sources in deep pencil-beam radio surveys. The study of the optical counterparts of the μJy population seems to indicate that the median R magnitude starts to decrease below 100 μJy. Spectroscopic classification of a sample of sources in this survey confirms the trend for an increasing fraction of star-forming galaxies over other systems down to ∼ 100 μJy.

The prospects for electron Bernstein wave heating of spherical tokamaks

Electron Bernstein waves are analyzed as possible candidates for heating spherical tokamaks. An inhomogeneous plane slab model of the plasma with a sheared magnetic field is used to calculate the linear conversion of the ordinary mode (O-mode) to the extraordinary mode (X-mode). A formula for the fraction of the incident O-mode energy which is converted to the X-mode at the O-mode cutoff is derived. This fraction is then able to propagate to the upper hybrid resonance where it is converted to the electron Bernstein mode. The damping of electron Bernstein waves at the fourth harmonic resonance, corresponding to a 60 GHz source on the Mega Amp Spherical Tokamak MAST [A. C. Darke et al., Proceedings of the 16th Symposium on Fusion Energy, Champaign-Urbana, Illinois (IEEE, Piscataway, NJ, 1995, Vol. 2, p. 1456)], is computed. For comparison, results are also presented for a lower frequency source, close to the fundamental electron cyclotron resonance. Both the fundamental and the fourth harmonic are shown to be so strongly absorbing that the electron Bernstein wave would be totally absorbed in the outer regions of the resonance. This feature implies that electron Bernstein wave current drive (on- or off-axis) could be very efficient.

Electron cyclotron resonance ion source for high currents of mono- and multicharged ion and general purpose unlimited lifetime application on implantation devices

The electron cyclotron resonance (ECR) ion sources were originally developed for high energy physic applications. They are used as injectors on linear accelerators and cyclotrons to further increase the particle energy via high charge state ions. This ECR technology is well suited for sources placed on a high voltage platform where ac power available is limited by insulated transformers. The PANTECHNIK family of ion source with its wide range of ion beam (various charge states with various beam currents) offers new possibilities and perspectives in the field of ion implantation. In addition to all these possibilities, the PANTECHNIK ion sources have many other advantages like: a very long lifetime without maintenance expense, good stability, efficiency of ionization close to 100% (this improves the lifetime of the pumping system and other equipment), the possibility of producing ion beams with different energies, and a very good reproducibility. The main characteristics of sources like Nanogan or SuperNanogan will be recalled. We will especially present the results obtained with the new Microgan 10 GHz source that can be optimized for the production of high currents of monocharged ion, including reactive gas like BF3 (2 mA e of B+) or medium currents of low charge state like 0.5 mA e of Ar4+. The latest results obtained with Microgan 10 GHz show that it is possible to drive the source up to 30 mA e of total current, with an emittance of 150 π mm mrad at 40 kV and also to maintain the production of multicharged ions like Ar8+.

Infrared Planetary Nebulae in the NRAO VLA Sky Survey

In order to construct a sample of planetary nebulae (PNe) unbiased by dust extinction, we first selected the 1358 sources in the IRAS Point Source Catalog north of J2000 declination δ = -40° having measured S(25 μm) ≥ 1 Jy and colors characteristic of PNe: detections or upper limits consistent with both S(12 μm) ≤ 0.35S(25 μm) and S(25 μm) ≥ 0.35S(60 μm). The majority are radio-quiet contaminating sources such as asymptotic giant branch stars. Free-free emission from genuine PNe should make them radio sources. The 1.4 GHz NRAO VLA Sky Survey (NVSS) images and source catalog were used to reject radio-quiet mid-infrared sources. We identified 454 IRAS sources with radio sources brighter than S ≈ 2.5 mJy beam-1 (equivalent to T ≈ 0.8 K in the 45'' FHWM NVSS beam) by positional coincidence. They comprise 332 known PNe in the Strasbourg-ESO Catalogue of Galactic Planetary Nebulae and 122 candidate PNe, most of which lie at very low Galactic latitudes. Exploratory optical spectroscopic observations suggest that most of these candidates are indeed PNe optically dimmed by dust extinction, although some contamination remains from H II regions, Seyfert galaxies, etc. Furthermore, the NVSS failed to detect only 4% of the known PNe in our infrared sample. Thus it appears that radio selection can greatly improve the reliability of PN candidate samples without sacrificingcompleteness.

Planetary Nebulae in the NRAO VLA Sky Survey

The 1.4 GHz NRAO VLA Sky Survey (NVSS) images and source catalog were used to detect radio emission from the 885 planetary nebulae north of J2000 declination δ = -40° in the Strasbourg-ESO Catalogue of Galactic Planetary Nebulae. We identified 680 radio sources brighter than about S = 2.5 mJy beam-1 (equivalent to T ≈ 0.8 K in the 45'' FWHM NVSS beam) with planetary nebulae by coincidence with accurate optical positions measured from Digitized Sky Survey (DSS) images. Total extinction coefficients c at λ = 4861 A were calculated for the 429 planetary nebulae with available Hβ fluxes and low free-free optical depths at 1.4 GHz. The variation of c with Galactic latitude and longitude is consistent with the extinction being primarily interstellar and not intrinsic.

Active Star Formation toward the Ultracompact HiiRegions G45.12+0.13 and G45.07+0.13

A multiwavelength study of the molecular cores containing the ultracompact (UC) H II regions G45.12+0.13 and G45.07+0.13 reveals a series of phenomenological differences that distinguish the age of these cores in terms of their development of high-mass star formation. First, we report the discovery of massive, bipolar molecular outflows from both UC H II regions. The G45.12+0.13 UC H II region lies centered on a spatially extended, 6 km s-1 outflow that we have mapped in the CO J = 2 ? 1, 3 ? 2, 6 ? 5,13CO 2 ? 1, and C18O 2 ? 1 transitions at the Caltech Submillimeter Observatory (CSO). The broad bipolar structure is optically thick in the 12CO line. The 13CO measurements imply a large outflow mass of 4800 M? (12% of the total cloud mass). Interferometric observations with the Owens Valley Radio Observatory (OVRO) millimeter array in the 13CO 1 ? 0 line resolve the gas into at least two outflows, one of which emanates from the 4.0 Jy, 110 GHz source identified with the UC H II region. An additional outflow is driven by an adjacent young, embedded object that contributes to the extended submillimeter continuum emission imaged with the CSO bolometer array camera. Lying in a separate core a few arcminutes away, the G45.07+0.13 UC H II region contains H2O masers and presents higher velocity (11 km s-1) yet more compact CO emission. An outflow has been detected in the CO 6 ? 5 transition, along with a compact submillimeter continuum source. OVRO observations in the CS J = 2 ? 1 transition confirm a compact outflow centered on the 98 GHz continuum source toward which infall is also seen in the form of redshifted absorption. The multiple outflows, higher CO antenna temperatures, more extended submillimeter and radio continuum emission, and lack of H2O masers all distinguish the core containing G45.12+0.13 as a more advanced site of massive star formation than the neighboring core containing G45.07+0.13.

Enhanced nucleation and growth of diamond thin films using a nanodiamond monolayer

It is well known that the nucleation density during diamond film growth can be enhanced by simply scratching the substrates. The abrading particles need not be diamond, as high nucleation densities have been reported on substrates treated with particles of SiC [1], BN [2] etc. However, preferential growth of diamond on diamond has also been reported when diamond is present on the substrate surface as a residue from the polishing [3, 4]. Providing diamond or other nucleation sites is essential as the diamond nuclei formed in the gas phase as a result of the homogeneous nucleation remain unstable until they have reached a certain critical size. This is because the addition of carbon atoms to the nucleus decreases the bulk contribution to the free energy but increases the surface contribution. Therefore, the nuclei formed from the gas phase under normal conditions are unlikely to survive long enough to have an adequately low surface to volume ratio [5]. Thus nucleation on untreated surfaces is slow and leads to a very slow growth rate of the film [6]. Different techniques have been utilized to enhance the nucleation and growth rate of diamond thin films during chemical vapour deposition (CVD). Nonabrasive techniques have been sought since the polishing process is generally manual and seldom exactly reproducible. Stoner et al. [7] used a combination of negative bias and high methane concentration at the beginning of the deposition run in order to produce an SiC layer followed by carbon cluster formation which eventually led to diamond nucleation. A nucleation density three to five orders of magnitude higher than with conventional polishing was obtainable. Several investigators have also successfully used bucky balls [8] and bucky tubes [9] for diamond nucleation. Hartnett et al. [10] used laser ablated amorphic carbon layer for diamond nucleation and reported a nucleation density of 106 cmy2. In this letter we report the growth of diamond films on Si substrates using a nanodiamond monolayer as the nucleation enhancement layer. Enhancements of almost an order of magnitude in the nucleation density and more than a factor of three in the deposition rate over conventional polishing techniques have been realized. The substrate treatment involved making a slurry of commercially available du Pont nanodiamond powder and methanol. The nanoparticles in the nanodiamond powder were typically 5–10 nm in size. The slurry was formed by mixing approximately 4 g nanodiamond powder in 1 l methanol. The substrates were then placed in this slurry such that the slurry covered the surface of the substrates, and the methanol was allowed to evaporate. By controlling the amount of nanodiamond powder in methanol it is possible to deposit a monolayer of the nanodiamond particles. The substrate was never mechanically abraded in this experiment. Diamond films were deposited in an ASTEX microwave plasma assisted CVD system, which has been described elsewhere [11]. The plasma contained 0.6% CH4 and H2 excited by a 2.45 GHz source with 1500 W power. Deposition was carried out at 850 8C substrate temperature and 500 sccm flow rate. For comparison, films were also deposited on Si substrates that had been mechanically polished with diamond paste. Films were deposited for 15, 30 and 240 min. Fig. 1b shows a SEM micrograph of a sample grown with the nanodiamond layer for 15 min. The nucleation density calculated from this micrograph was 1:5 3 108 cmy2. Parallel samples grown on the Si substrates that were mechanically polished using diamond paste gave a nucleation density of 1:7 3 107 cmy2 after 15 min growth, as shown in Fig. 1a. After 30 min growth the nucleation densities were 2:7 3 109 and 1:8 3 108 cmy2 on the substrates with a nanodiamond layer and on mechanically polished substrates, respectively. Films grown for longer times were used to measure the deposition rate. The deposition rate for the diamond film with the nanodiamond interlayer was measured to be 1.3 μm hy1 as compared to 0.4 μm hy1 obtained for the deposition on the polished substrate under identical deposition conditions. Fig. 2 shows Raman spectra obtained from diamond films on the substrates with nanodiamond interlayer and with mechanically polished substrates. The spectra are virtually identical, indicating similar quality film growth in both cases, despite a very high deposition rate for the sample with the nanodiamond nucleation layer. In both cases, in addition to the sharp peak at 1332 cmy1 attributed to the crystalline sp3 fraction of the film, there is a broad peak

Fibre-supported optical generation and delivery of 60 GHz signals

A novel ‘frequency quadrupling’ technique for the optical generation and delivery via fibre of modulated 60 GHz band millimetre-wave signals is described. The technique requires only microwave frequency capability for the optical modulator and drive electronics, and these are readily available commercially. The frequency quadrupling technique is demonstrated experimentally with a high spectral purity 60 GHz signal obtained using a 15 GHz source and optical modulator.

Multiple wavelength observations of an off-limb eruptive solar flare

The eruptive prominence and limb flare which occurred at 1454 UT on June 20, 1989 is described and analyzed. This event was observed by many different instruments providing an unusual amount and variety of data: images at 1.4 GHz, 37 GHz, and H-alpha, and spectra in hard X-ray, soft X-ray, and radio frequencies. This array of data makes it possible to explore the relationships between flare and eruptive prominence emissions at different wavelengths. VLA images at 1.4 GHz show changing sources in a set of high (about 10 exp 10 cm) coronal loops associated with the erupting prominence. We use a full gyrosynchrotron code to model a 1.4 GHz source early in the flare as a large coronal loop. The model results lead us to conclude that the initial acceleration occurs in smaller, denser loops which also produce the flare's hard X-ray emission. We also present evidence that a source at 1.4 GHz later in the event is due to second-harmonic plasma emission. This source is adjacent to a leg of the prominence and comes from a dense column of material in the magnetic structure supporting the prominence.

Observations of strong microwave absorption in collisional plasmas with gradual density gradients

Strong microwave absorption was observed when a 10 GHz source illuminated an underdense collisional plasma that had a density gradient scale length several wavelengths long. Significant reductions in angular scattering and cross-polarized components were also observed. These experiments confirm that absorption was the dominant process. The plasma was created by the photoionization of tetrakisdimethylaminoethylene molecules seeded into atmospheric pressure helium. Sparkboard arrays provided the intense vacuum ultraviolet ionizing radiation. Plasma density profiles were measured using transverse scans of 9.7 GHz probe microwaves and were found to approximate an Epstein profile. The absorption at 10 GHz by this plasma was as large as 28 dB in direct backscattering and 15–20 dB when orthogonally polarized microwaves were launched and detected. The peak absorption scales with sparkboard energy in a way that suggests that electron-ion recombination is the dominant electron-loss mechanism at high plasma densities.

A 1.4 GHz source survey in an area without nearby rich galaxy clusters

The paper reports on 1.4 GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z less than 0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5 mJy, in an area of about 12 sq deg. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z greater than 0.4 (tabulated by Gunn, Hoessel, and Oke, 1986). Source positions are compared with those from an optical catalog and mild correlations on angular scales of order 1 arcmin are found. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z = 0.1, even though there are no rich galaxy clusters in this redshift range.

Source d'ions lourds multicharges caprice 10 GHz pour tous les elements metalliques et Gazeux

A new compact multiply charged E.C.R. ion source completely enclosed by an iron return yoke is described. A new coaxial 10 GHz microwave accessibility is operating. This allows a very compact two stages source in an entirely removable vacuum chamber and a very easy increasing possibility of the axial magnetic field value. Then two different working modes are possible. A classical mode ( ω ce = ω rf, 100% cw, rf power 300 W, coils supply 20 kW) gives same performance than all the other reliable larger 10 GHz sources. A second mode (100% cw, rf power 600 W, coils supply 33 kW) operates with an additional resonant surface ω ce = 2 ω rf and increases by a factor 3 or 4 all currents on high charge states. Total extraction current is multiplied by a factor of 4 just as it would do by using a classical 20 GHz source by increase in density. This new resonant surface is unfortunately stopped in its radial part by the wall of the vacuum chamber due to a too low 10 GHz sextupole (0,4 T). Presently a better sextupole (0,8 T) is being built in order to work with both whole resonant surfaces inside the plasma chamber and perhaps so to improve charge states distribution by rising the plasma life time. On the other hand both the removable vacuum chamber and the coaxial rf feeder are well fitted to produce all metallic ions in long run and high intensity by working without any insulator inside the plasma chamber and by a good cleaning possibility. One shows cw spectra of 10 metallic elements from Al to Au and one can observe an exponential decrease for Ca, Ag and Au. This remark indicates a possible easy way to yield high charge states of all metals. One can expect to regulate all the easiest elements like Al, Si, Fe, Ni, Mo, Ta and W for 100 h. For example a good (within 1%) regulation of a 15 μA 56 26Fe 7+ for 10 h is partly shown.