The uplink logic automatically selects the integrating capacitance based on estimated continuum and line fluxes. If an observation contains lines that fall in different flux regimes, the largest applicable capacitance will be chosen for the entire observation. If lines in the same observation fall in different flux regimes, it is recommended to split the observation into separate observations per flux regime. The HSpot Time Estimator Message (click on "Observation Estimation / PACS Time Estimator Messages") indicates if other than the default capacitance has been selected for a given combination of lines. Please note, a single bright line could trigger capacitance switching in both read and blue channels, i.e. capacitances are always kept in synch between the two channels. In case a bright red line is grouped together with faint lines in the blue channel then the observation will be sub-optimal in the blue. In such a case it is recommended to regroup lines per channel in two separate AORs.

Spectral regions affected by leakage are discussed in Section 4.8. The measured spectrum in these regions may contain superimposed flux originated in the parallel channel, the interpretation of spectral features (unresolved or continuum fluxes) should be avoided without consulting a PACS expert (i.e. contact Helpdesk).

The default mode for point-source spectroscopy, a single pointing on the source. The integral-field concept allows simultaneous spectral and spatial multiplexing for the most efficient detection of weak individual spectral lines with sufficient baseline coverage and high tolerance to pointing errors without compromising spatial resolution. The PACS spectrometer arrays have 5 by 5 spatial pixels covering a 47 by 47 arcseconds field-of-view respectively, both channels viewing almost identical positions on the sky. The line flux from a point source object will always be collected with the filled detector array, with most the source flux falling on the central pixel. Therefore, for the plain detection of a line source, one pointing is sufficient for a point- or compact source.

This mode allows the observer to set up a pointed observation in combination with chopping/nodding or unchopped grating scan techniques.

	Warning
	HSpot v5.0 and later versions allow the reading of AORs in 'Pointed with dither' mode but time estimation has been disabled and submission to HSC is not possible. This mode has been decommsissionned.

It has been proven during the Performance Verification Phase that flux reconstruction from a single pointed observation is as good as in dithering mode, therefore dithering option is not recommended anymore. For sources with a well confined photocenter (point- or compact sources), the pointing mode can be changed from 'Pointed with dither' to 'Pointed'. To maintain the observation integration time, nod repetition and/or scan repetitions should be increased until the original observing time is reached. Nod or range repetition x 3 should be the appropriate change for most observations. Observations requiring spatial oversampling should use a minimum 2x2 size raster with recommended step sizes.

This mode allows the observer to set up a raster map observation in combination with chopping/nodding or unchopped grating scan techniques.

In chop/nod mode, the map can only be defined in instrument coordinates, and the map size shall be restricted to 6' by 6' to obtain clean offset positions with the large chopper throw for each raster position. The user is therefore advised to build a square raster map to be position angle independent, in other words to define a map with the same number of raster points and step sizes on the X and Y axis.

	Note
	Raster lines are performed along the Z-axis (in contrast to photometer raster map where raster lines are along the Y-axis), i.e. perpendicular to the chopping axis, as can be visualized in HSpot with the AOR overlay functionality.

In unchopped grating scan mode the map can be defined in instrument- as well as sky coordinates, with a maximum size of 2 degrees, and sparsely sampled maps are possible.

	Warning
	In mapping mode, the sensitivity given by HSpot refers to each single raster point and does not take into account internal redundancy. The sensitivity shall increase roughly with the square root of the redundancy factor (number of times a sky pixel is seen by a spectrometer spatial pixel).

6.1.5.1. Map orientation reference frame

The recommended raster step/line size settings (see below) have been optimised only for zero degree map orientation in instrument coordinates. In case of applying sky reference frame then optimal spatial sampling cannot be guaranteed because the PACS footprint rotation with respect to the raster line orientation depends on the position angle of the detectors footprint (determined by the day of the observation). The sky reference frame can be selected only in unchopped grating scan mode. Please note, in unchopped grating scan mode the HSpot default option is 'sky' reference, but we highly advise to switch to 'instrument' mode except for cases described in Section 6.1.5.2.

Note

Time constraints as well as the chopper avoidance angle may be used to put restrictions on the map orientation angle if the map is defined in 'instrument' reference frame. The time constraint can indirectly limit the array position angle in the optimal range, while the chopper avoidance can be used to avoid a certain chopping direction with respect to the target position (see details in the HSpot Users Manual). Map orientation direction restrictions are possible only for targets at high ecliptic latitude, here the spacecraft orbit may result different position angles at different observing epochs.

6.1.5.5. Nyquist sampling map of extended objects

For extended objects, mapping with oversampling, i.e. with step size smaller than one spaxel, may be very time consuming. Therefore this mapping strategy is suggested with step sizes larger than one spaxel, but such that the beam is Nyquist sampled. Taking into account that what is defined as raster point step in HSpot corresponds to the spacecraft Z axis, and the line step to the Y axis, the recommended raster step sizes (see ???) for Nyquist sampled maps of larger areas translate to the following HSpot settings:

• Blue: point step=16.0", line step =14.5"

• Red: point step=24.0", line step =22.0"

Figure 6.2.  Spatial sampling by all PACS spaxels when using a 5x5 raster with step size 14.5"/16" for the blue (left) and a 3x3 raster with step size 22"/24” for the red (right)

	Note
	For oversampled maps (Section 6.1.5.5 and Section 6.1.5.6) the optimum separation between raster points has been optimised to a reference beam size in the blue and red channels. In case an AOR contains a mix of blue and red lines/ranges then it is recommended to adopt the blue settings.

This mode is called "Chopping/nodding" in the "observing mode settings" panel of HSpot. The chopping technique is the standard way of observing with the PACS spectrometer, this mode is recommended especially for faint lines (below 4-5 Jy peak-to-continuum) combined with faint- or bright continuum. Both line flux and continuum level can be recovered from the data. The mode could be used in a reliable way only if clean off-fields are available within a 6' radius with respect the target coordinates.

An observing request can contain up to 10 spectral line scans across different bands with the same fixed order selection filter wheel position. For each observer defined wavelength in the PACS Line Editor, the spectrometer performs grating scans with an amplitude such that a given wavelength is seen successively by all 16 spectral pixels. The sampling density per resolution element is higher than 3 samples per FWHM of an unresolved line at all wavelengths with 43, 46 and 48 grating steps in the first, second and third order respectively (see scan parameters in Table 6.2). A single grating scan is repeated in two directions. This up/down scan can be repeated up to 10 times for a single line. Table 6.3 shows the wavelength range covered in the different bands.

At every grating position, the detector signal is modulated between on and off source via an [on-off-off-on]-[on-off-off-on] chopping pattern. In order to take advantage of the best spectrometer sensitivity, at every chopper plateau two 1/8 second integrations of the photoconductor signals are recorded. These integration ramps of 1/8 second length are fitted on-board PACS, therefore the signal transmitted to the ground is represented by the slope of the ramp in terms of [ADU/reset interval].

The observer can choose a chopper throw of "Small", "Medium" and "Large" what refering to 6', 3'or 1.5' respectively. The apparent chopper throw is curved on the sky. This rotates the on-source spectral footprint in the two nod positions, and this rotation becomes larger with increasing chopper throw (see Section 4.5).

	Note
	It is recommended to select the "Small" (1.5') chopper throw if applicable for the target (i.e. well isolated point-sources) in order to reduce the effect of field-rotation between the two chop positions (see Figure 6.3).

Figure 6.3.  Spatial footprint layout of the chop/nod observing mode: two chopper positions are shown for nod A and B. The zoom in the on-source position reveals the field-rotation between the two chop positions.

Note

In case some disturbing sky features would fall in within the chopper throw radius around the target, the observer has to consider to setup a chopper avoidance angle constraint. The angle can be specified in equatorial coordinates counterclockwise with respect the celestial north. The avoidance angle range can be specified up to 360 degrees with a minimum range of 15 degrees, to avoid too much restrictions on scheduling. Setting up a chopper avoidance angle requires an additional constraint on mission planning, therefore this parameter should have to be used only for observations where it is absolutely necessary.

The sequence of line scans is repeated at two nod positions of the telescope. In the second nod position (nod B), the source is located in the off chopping position of the first nod (nod A). With this technique, one can eliminate the telescope background what happens to be different at the optical angle of the two chop positions: F(observed) = [NodA(on-off)] + [NodB(on-off)] / 2 = [(T2+F(source)-T1] + [(T1+F(source)-T2] / 2 = F(source), where T1 and T2 are the telescope background fluxes at the two chopper positions. (In this term we assume the sky background is negligible compared to the telescope background.) The nod sequence can be repeated within one observation to increase the depth of the observation. Nod cycles are repeated in a way that A-B slew times are minimised, for instance, in case of two repetitions the spacecraft follows the pattern: [A-B-B-A]. In chop/nod mode in total, one half of the science time is spent on-source. The principle of line spectroscopy is illustrated in the diagram of subsequent instrument and spacecraft observing blocks in Figure 6.5.

	Note
	For low number of repetitions (up to 5-6) it is recommended to repeat line scans (increase line repetition factor), while for deeper observations line repetitions should be combined with a number of nod cycles.

Figure 6.4.  At each grating position in an up/down scan 16 ontegration ramps are taken (plus 1 for synchronisation at the begnning). The ABBA sequence represents a chopper [on-off-off-on] cycle which is repeated two times. The duration of such a grating plateau is [8 integrations] x [1/8 sec integration time] x [2 ABBA cycles] = 2 seconds.

Figure 6.5.  Instrument observing blocks are shown for a typical chop/nod measurement combining two lines with single repetition in B3A and a third line with two repetitions in band R1 (3rd + 1st orders setting). Line repetitions adjust the relative depth required for spectral lines, while the number of observing cycle is used to repeat the entire nodding cycle. In the bottom the spatial layout of the chop/nod scheme is sketched. Note, the raster patterns has been distorted for better visibility, in real observations, the nod slew is significantly larger than the raster step size and nodding direction is enforced along the raster columns (vertical direction).

The full wavelength range covered by the scan and the range covered to the highest sensitivity, i.e. the wavelength seen by all 16 spectral pixels are shown in Table 6.3 and compared with respective FWHM of the spectrometer at these wavelengths, for an unresolved line. The spectral coverage in line spectroscopy modes is shown in Figure 6.6. The reference for the wavelength range as specified in HSpot is spectral pixel 8, i.e. the predefined range is not covered by all spectral pixels, and the actual range in the data has S/N going up at the edges.

The spatial layout of a pointed measurement is shown on Figure 6.7 where the 25 spaxels for the foure chop/nod position are projected onto the sky.

Chopping and nodding is imposed by the design of the AOT, in other words if chopping/nodding is deselected, the unchopped grating scan is selected instead, as both observing techniques are mutually exclusive.

Figure 6.6.  Visualization of the line scan AOT on an unresolved PACS line (here given by a Gaussian). The grating step size and number of grating positions used is the nominal one currently coded in AOT design for standard "faint lines" summarized in Table 6.2. Top row is for a blue line at 60µm; bottom row is for a red line at 205µm. In bright line mode, grating step sizes are identical but the instrument scans over only the 10 central positions. These scan patterns are identical for chopped- and unchopped modes.

Figure 6.7.  The PACS spectrometer footprint of a chop/nod pointed observation is shown for the blue band. The four fields of nod A and B positions combined with chop on- and off fields are plotted as well as the instrument boresight (grey) and target position (red). In this example observation large chopper throw (6') was used which is a result of a symmetrical chopping pattern around the instrument boresight.

This mode is devoted to bright lines where it is not needed to spend as much time per line as in the standard chopping/nodding mode with a single repetition. Up and down grating scans are performed but only with 10 grating steps, i.e. the on-sky time about 3-4 times shorter than in the standard chopping/nodding mode depending on the band. A comparison of bright line mode scan parameters can be found in Table 6.2.

The observing efficiency of this mode is rather poor because of fixed incompressible overheads (nod slew time and instrument overheads). The minimum total observing time (one line, one cycle) is 303s versus 583s in the standard chopping/nodding, while it is about twice less sensitive: the sensitivity ratio per resolution element in the highest sensitivity part of the coverage is about 0.6. (Sensitivity ratio is driven by the respective oversampling factors, sqrt(10 / 27.9)) If several lines are observed the modes becomes more attractive, but line repetition factor as well as nodding cycles should be equal or less than 3.

In bright line mode, even for unresolved lines, the central 3 pixels in a 16 pixel module do not "see" the continuum, they scan over the line profile only. This could make difficult a proper response correction as no flat continuum level can be determined for all the pixels.

	Note
	Since the bright line mode scans about 1/4th of the wavelength range scanned in faint line mode for broadened lines this might limit the wavelength extent of the baseline measured.

The unchopped grating scan is an alternative to the chopping/nodding mode if by chopping to a maximum of 6' the off position field-of-view cannot be on an emission free area, for instance in crowded-fields or for spectral line mapping of extended objects with diameter larger than 5' respectively. The direct way of acquiring data raises limitations on the applicable flux regime with respect to the standard chop/nod mode. This mode is not recommended for faint lines, target lines needs to be above typically ~1 Jy peak-to-continuum and the continuum level can be recovered in a reliable way only for bright sources, i.e. at a minimum continuum level of ~ 20-30 Jy.The continuum level can be determined by off-position subtraction which could efficiently eliminate the telescope background for bright objects.

6.1.8.1. Unchopped faint line mode

In this default version of the unchopped grating scan mode, the line is scanned with the same grating step as in chopped line spectroscopy, i.e., every spectral pixel samples at least every 1/3 of a resolution element. The number of grating steps is fixed to 75 irrespective the spectral band in which the line is observed. Other grating scan parameters and block duration are shown in Table 6.2.

A key element in the unchopped mode is to make this technique robust against instantaneous responsivity changes caused by cosmic ray hits in the Ge:Ga detector pixels. For this purpose, the up/down grating scan have been made much faster than in the chopped mode, and every line repetition requested by the observer is doubled internally by PACS. On every grating position, four integration ramps are taken. Each integration lasts 1/8 s, resulting in a grating scan which is four times faster than the one in chop mode.

The example of an observing block sequence of the unchopped grating scan mode is sketched in Figure 6.8. In the on-source block, the observer defined line repetitions are internally multiplied by two, i.e. a single repetition is made of two fast scans. The on-source integration time in this mode is half the time PACS spends on-source in the chopped mode (including both nod positions).

In pointed mode, following an on-source block the spacecraft slews to an off-position within two degrees radius with respect to the target coordinates. The off-position has to be carefully selected for an efficient subtraction of the telescope background. Ideally, the background sky emission towards the target and towards the off-position is at the same level respectively, and the background field is free of confusing structures (i.e. the 25 spaxels see a similar level of sky emission).

The off-position is always executed with a single repetition, irrespective what the observer has defined for line repetition factor in the PACS Line Editor. This means, the duration and signal-to-noise in the off-position blocks will be lower than the on-target block, if line repetition factor has been set larger than one.

Note

The repetition cycle has to be used to increase the exposure, the entire on-off block is repeated as is in the chopped mode. For instance, in two cycles the spacecraft follows an [ON-OFF-OFF-ON] pointing sequence between the two positions. For deep observations, if necessary, the off-position duration could be kept identical to the on-source duration by specifying single line repetitions and higher number of observing cycles. However, this parameterization is inefficient in terms of slewing overheads.

	Note
	While the scheme in the block diagram Figure 6.8 can be executed, it may turn more advisable to rather do this line by line, particularly for rasters with not too frequent off positions.

	Note
	A shorter integration time in the OFF-position results in a RMS noise of the reference continuum higher than that of the source continuum. To avoid to increase the RMS noise when subtracting the OFF-position, the OFF-position data can be binned using larger wavelength intervals. In case of flat continuum, a single value can be computed for the reference continuum.

Figure 6.8.  Instrument observing blocks are shown for a typical unchopped grating scan measurement combining two lines with single repetition in B3A and a third line with two repetitions in band R1 (3rd + 1st orders setting). Line repetitions adjust the relative depth required for spectral lines, while the number of observing cycles is used to repeat the entire on-off cycle. In this example, the off-position is only 6' away from the target what results only short on-off slewing overhead.

In raster mapping mode the observing block sequence is similar to the chopped mode but here the observer could define the number of raster positions to visit before moving to the off-position.

	Note
	In mapping mode, the observing cycle is repeating the entire raster. At least one OFF-position has to be specified for a single cycle, i.e. the number of raster positions to visit before moving to the OFF-position has to be equal or lower than the number of raster positions ([num. raster lines] x [num. of raster points])

In raster mode, PACS executes an obligatory OFF-position before the first science block starts at the first raster position. For instance, in case of a 2x2 raster, with a single cycle and with an off position request after 2 raster positions, the following spatial pattern will be executed: [OFF-ON-ON-OFF-ON-ON-OFF]. The same raster with two cycles: [OFF-ON-ON-OFF-ON-ON-OFF-ON-ON-OFF-ON-ON-OFF].

6.1.8.2. Unchopped bright line mode

This bright-line option has been made available in HSpot version 5.3.1 and later for science cases where very high signal-to-noise (S/N > 100) line detections are expected applying a single line repetition factor. For such bright targets, the integration time can be kept shorter than as is in the default faint-line mode, even on the expense of compromised observing performance.

	Warning
	At the time of the GT2 call, precise sensitivity numbers have not yet been characterized for the bright line mode, however, preliminary validation results indicate a loss of sensitivity not more than a factor two comparing to the default faint-line mode. For more up-to-date information please contact the Herschel Science Centre Helpdesk.

In this mode, grating scan parameters and observing logic remain unchanged, except the number of grating steps visited by a single scan. Instead of applying the default 75 steps, a bright line scan is done through 50 steps, resulting a factor 1/3 reduction in integration time. The shorter duration scan is therefore achieved via a shorter wavelength coverage, the scan speed (number of integration ramps per grating position) has not been changed. Due to instrument and spacecraft overheads the 33% gain in integration time does not apply to the total duration of a bright line AOR. Typically, a bright line AOR is shorter by 25-30% than its faint-line homologue.

	Note
	The shorter wavelength coverage on both sides of the line profile may result a higher uncertainty in the continuum level reconstruction.

The wavelength switching technique/mode is an alternative to the chopping/nodding mode, if by chopping to a maximum of 6 arcminutes, the OFF position field-of-view cannot be on an emission free area, for instance in crowded areas.

	Warning
	The wavelength switching mode has been deprecated in HSpot v5.0 and later versions. For crowded-field spectroscopy, and in more general, for science cases where chopping is not possible it is advised to use the unchopped range scan mode instead. Observers with AORs in wavelength switching mode could still read these observations in HSpot but time estimation is not possible any further.

In wavelength switching mode, the line is scanned with the same grating step as in chopped line spectroscopy, i.e., every spectral pixel samples at least every 1/3 of a resolution element. In wavelength switching we refer to this step as a dither step. At every dither step, the signal is modulated by moving the line over about half of the FWHM. This allows one to measure a differential line profile, canceling out the background (Figure 6.9). The modulation on every scan step follows an AABBBBAA pattern, where A is a detector integration at the initial wavelength, and B is a detector integration at the wavelength switching wavelength. This cycle is repeated 20 times in one direction, and repeated in the reverse wavelength direction. The switching amplitude is fixed for every spectral band.

In order to reconstruct the full power spectrum, a clean off- position is visited at the beginning and the end of the observation. On this position the same scan is performed. In between, the scan is performed at two or more raster positions.

Figure 6.9.  Reconstruction of emission line flux in the differential wavelength switching mode (by fitting a differential Gaussian).

Wavelength switching can be used for large extended sources since no clean reference is needed. But it shall be used with caution: by definition this technique eliminates the continuum information. Besides the baseline estimates, line profiles are not be reliable if: