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Atmospheric Measurement Techniques An interactive open-access journal of the European Geosciences Union
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AMT | Articles | Volume 13, issue 10
Atmos. Meas. Tech., 13, 5681–5695, 2020
https://doi.org/10.5194/amt-13-5681-2020
© Author(s) 2020. This work is distributed under
the Creative Commons Attribution 4.0 License.
Atmos. Meas. Tech., 13, 5681–5695, 2020
https://doi.org/10.5194/amt-13-5681-2020
© Author(s) 2020. This work is distributed under
the Creative Commons Attribution 4.0 License.

Research article 26 Oct 2020

Research article | 26 Oct 2020

A technical description of the Balloon Lidar Experiment (BOLIDE)

A technical description of the Balloon Lidar Experiment (BOLIDE)
Bernd Kaifler1, Dimitry Rempel1, Philipp Roßi1, Christian Büdenbender1, Natalie Kaifler1, and Volodymyr Baturkin2 Bernd Kaifler et al.
  • 1Deutsches Zentrum für Luft- und Raumfahrt, Institut für Physik der Atmosphäre, Oberpfaffenhofen, Germany
  • 2Deutsches Zentrum für Luft- und Raumfahrt, Institut für Raumfahrtsysteme, Bremen, Germany

Correspondence: Bernd Kaifler (bernd.kaifler@dlr.de)

Abstract
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The Balloon Lidar Experiment (BOLIDE) was the first high-power lidar flown and operated successfully on board a balloon platform. As part of the PMC Turbo payload, the instrument acquired high-resolution backscatter profiles of polar mesospheric clouds (PMCs) from an altitude of  38 km during its maiden  6 d flight from Esrange, Sweden, to northern Canada in July 2018. We describe the BOLIDE instrument and its development and report on the predicted and actual in-flight performance. Although the instrument suffered from excessively high background noise, we were able to detect PMCs with a volume backscatter coefficient as low as 0.6×10-10 m−1 sr−1 at a vertical resolution of 100 m and a time resolution of 30 s.

1 Introduction
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For several decades light detection and ranging (lidar) has been the only technology which allows for profiling of the neutral atmosphere from the troposphere to the upper mesosphere and lower thermosphere. Although the basic principle has not been changed since the first experiments using powerful searchlights as a light source, it was the invention of the laser which facilitated the technological breakthrough and adoption of the lidar method for atmospheric research. First observations of tropospheric clouds by lidar were reported in the 1960s and were soon followed by observations of stratospheric aerosols (e.g., Collis1965, 1966; Schuster1970). However, it took another decade before the technology became mature enough to allow for measurements of air densities with sufficient precision and accuracy for the retrieval of mesospheric temperature profiles by hydrostatic integration (Hauchecorne and Chanin1980).

The push to ever greater heights and better time and altitude resolutions was mainly hindered by two things. First, the density of air decreases exponentially with altitude, causing the lidar return signal to decrease exponentially with altitude too. Second, in the picture of geometric optics the scattered light forms spherical waves, resulting in the lidar return signal decreasing with the range squared (or altitude squared in the case of a vertically looking lidar). Both factors are responsible for the rapid deterioration of the received signal and put a natural limit on the altitude where the desired signal fades into background. One pragmatic, although from a technical point of view less straightforward, answer to this problem was power scaling of lidar systems, i.e., the use of more powerful lasers, larger telescopes, and more sensitive detectors (von Zahn et al.2000; Sox et al.2018). Another more creative solution was first demonstrated in the late 1970s. Gibson et al. (1979) showed that mesospheric temperature could be retrieved from probing of the Doppler-broadened sodium D1 and D2 lines (Krueger et al.2015). Although the sodium density within the metal layer (approximately 80–100 km altitude) is only on the order of a few thousand atoms per cubic centimeters and thus much smaller than the air density at these altitudes, the sodium fluorescence signal is nevertheless much stronger than Rayleigh scattering due to the  16-orders-of-magnitude difference in the scattering cross sections. The downside of these so-called metal fluorescence (or resonance) lidars was the technical complexity of the lasers. While Rayleigh scattering is observed for any wavelength, fluorescence lidars require precise tuning of the laser wavelength to the absorption line of the probed metal atoms. This requirement resulted in bulky and less reliable lasers which were often cumbersome to operate. Hence, metal fluorescence lidars never became as widely used as Rayleigh lidars.

Another option to boost the lidar return signal is to decrease the distance between the lidar and the probed volume. As mentioned before, the lidar return signal decreases with the distance squared when disregarding the exponential decrease in air density. Thus, for example, a lidar flying at 40 km altitude and probing a volume at 80 km experiences a 4-fold increase of the desired signal over a ground-based lidar probing the same volume. Additionally, such a lidar gains about 20 % in signal due to avoiding the significant optical extinction caused by scattering in the lower atmosphere. Furthermore, with more than 99 % of the air below, the upward-looking flying lidar collects much less scattered sunlight than its ground-based counterpart. The low solar background would permit the flying lidar to make observations in full daylight without the ultra-narrowband optical filters required in receivers of ground-based lidars. Omitting the filters not only considerably simplifies the optical design of the lidar but at the same time also increases the overall transmission of the instrument. The latter facilitates the use of even smaller lasers and/or telescopes while still achieving the same signal level as large ground-based instruments. Taking into account the above considerations, the concept of a compact but powerful balloon-borne mesospheric lidar appears feasible and enticing. The greatest benefits from such an instrument are expected for studies which require observations in daylight, for example high-resolution profiling of polar mesospheric clouds (PMCs).

With the mass and power requirements met (typically a few hundred kilograms and up to 1 kW for large balloon payloads), the technological challenges of getting a lidar to work in the near-space environment are still formidable in comparison to ground-based systems. The balloon experiment has to withstand low pressure, intense solar radiation, and extreme temperatures ranging from −60C encountered during ascent and descent to >100C in sunlit conditions at floating altitude. With not enough air pressure for convective cooling, the only means to dump waste heat generated by the instrument is to radiate it into space. Any instrument which dissipates a significant amount of electrical power requires a radiator for cooling and thermal shielding similar to satellites. Furthermore, on long-duration balloon flights communication between the ground station and balloon payload typically relies on satellite links, which may not be available all the time and are severely limited in bandwidth. Thus, the experiment is required to have the capability to run autonomously for at least some periods and needs to incorporate fault protection routines to deal with potential anomalies. Hence, the design of a balloon lidar system faces challenges which are very similar to those of satellite instruments. While mass, volume, and power requirements may be less restrictive for a balloon instrument, thermal control is actually more challenging. In addition to radiative heating and cooling experienced in (near) space, the balloon instrument has to cope with a variable amount of (forced) convective cooling, in particular during the ascent and descent of the balloon through the cold tropopause. One of the biggest differences, also from a management point of view, is that balloon projects typically operate on a much smaller budget and compressed schedule.

The roots of the Balloon Lidar Experiment (BOLIDE) project go back to the 12th International Workshop on Layered Phenomena in the Mesopause Region (LPMR) held in Boulder, USA, in 2015. David C. Fritts (GATS Inc., Boulder Division) gave a presentation on a recently selected NASA long-duration balloon mission carrying a suite of narrow- and wide-field cameras for imaging of PMCs. The mission was called PMC Turbo and the payload was to be launched from McMurdo in Antarctica in the 2017–2018 season on a flight lasting approximately 14 d (Fritts et al.2019). Also present during the workshop was B. Kaifler (German Aerospace Center, DLR), who proposed to augment the payload with a lidar for near-vertical profiling and altimetry of PMCs, information which cannot be retrieved from the planned imaging experiments but is critical for the interpretation of the acquired images. The proposal led to an agreement between NASA and DLR in January 2016, when NASA formally accepted the balloon lidar experiment as a contributed instrument.

Less than a year before the anticipated launch date it became clear that PMC Turbo would be unable to fly from McMurdo in the 2017–2018 austral summer, and NASA offered a launch from Esrange, Sweden (Fritts et al.2019). Because BOLIDE was specifically designed for a flight in Antarctica and all design work was completed before the launch site was moved, in the following we will describe the original mission and mission requirements as much as possible and point to changes implemented in light of the flight in the Northern Hemisphere where necessary.

In addition to the science objectives, the BOLIDE project served also as “proof of concept” for various technologies, for example operation of an efficient single-loop liquid cooling system on a balloon platform. The instrument was also remarkable for its rapid development cycle and its low cost relative to other balloon instruments of similar complexity. In this regard BOLIDE will also hopefully serve as a pathfinder for future balloon instruments much like the Mars Pathfinder mission did for robotic space missions (Golombek et al.1999). Before BOLIDE there was only one previous attempt to fly a high-power lidar on a balloon. The Balloon Winds payload, a technology demonstrator for a future satellite mission, was, however, lost during a launch mishap, and no in-flight data were collected (Dehring et al.2006).

2 Requirements and early design phase
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In the early conceptual design phase following the LPMR workshop, requirements were defined as follows. (1) The lidar is to provide PMC backscatter profiles with higher resolution than and similar PMC detection threshold to the ground-based ALOMAR Rayleigh–Mie–Raman (RMR) lidar, i.e., 30 s temporal and 100 m vertical resolution with a detection threshold of ΔβPMC=1×10-10m-1sr-1. For comparison, Fiedler et al. (2011) used 14 min, 150 m, and ΔβPMC=1×10-10m-1sr-1 for processing ALOMAR data. Kaifler et al. (2013) processed data acquired with the same instrument at 30 s and 40 m resolution, but no information on the detection threshold is provided. (2) The lidar is to provide temperature profiles below the PMC layer in the range  50–75 km. (3) The average power consumption is <700W and the mass should not exceed 150 kg, and (4) the height of the telescope is limited to 1.6 m. The latter resulted from the maximum permissible height of the gondola and the constraint to place the telescope in the shadow zone of the gondola. From the very beginning PMC Turbo was designed as a pointed payload, using an azimuth rotator to track the Sun and turn the science instruments in an anti-solar direction. With the solar array mounted on the Sun-facing side of the gondola and science instruments placed on the opposite side, a permanent shadow zone is created behind the solar array which protects the instruments from direct solar radiation (see Fig. 4). (5) The viewing direction is limited to >26 off zenith. This requirement follows from the size of the balloon above the gondola and the length of the flight train, as for obvious reasons the laser beam is not allowed to hit the balloon. The requirements are summarized in Table 1.

Table 1BOLIDE instrument requirements and actual performance. The PMC detection threshold is defined for 30 s time resolution and 100 m vertical resolution.

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For the early design studies DLR's mobile ground-based lidar systems served as a starting point for performance studies as well as for weight and power calculations (e.g., Kaifler et al.2015). These lidars use diode-pumped solid-state lasers with 12 W output power at 532 nm wavelength as a light source and a 508 mm diameter fiber-coupled f∕2.4 mirror as a receiving telescope. While the optical power of the laser was certainly sufficient, the electrical power consumption and a projected mass of  40 kg for the laser alone became a problem. The real showstopper was, however, the need to pump deionized water through the laser pump chambers for cooling. Not only would the use of water as a primary coolant require a dual-loop cooling system, as water in the external radiator is likely to freeze during the ascent through the cold tropopause, but it would also result in guaranteed destruction of the laser upon landing. Recovery of the payload on the Antarctic Plateau is estimated to take a few days at best, and during that time the payload is subject to the cold Antarctic environment, with the laser eventually reaching subzero temperatures. These problems led to the selection of a less powerful but passively cooled laser which could be mounted on a cooling plate instead of running coolant directly through the pump chambers.

Further significant design changes included the selection of a smaller telescope to satisfy the height criterion and the reduction of the telescope field of view (FOV) to 165 µrad. The latter was motivated by the corresponding reduction in the solar background which is proportional to the FOV squared. The requirement for ground tests in daylight followed from selection of the launch site. Because the lidar would be disassembled before shipment to McMurdo, Antarctica, and deployment was scheduled to take place in November, when the Sun is already up 24 h a day, tests in daylight were seen as the only means to carry out a full system test before the actual balloon launch. The use of a narrow-band etalon in the receiver for filtering out the solar background was dismissed early on because this would have required a narrow-band transmitter, i.e., a seeded laser. Since the BOLIDE instrument was regarded as the first test of a mesospheric lidar system on a balloon, it was designed for simplicity and reliability and thus lacked a seeded laser. Without any possibility to sufficiently filter out the solar background, testing the lidar in daylight could only be achieved by inserting neutral-density filters into the optical path of the receiver. That obviously also attenuates the wanted signal, but it reduces the total signal – i.e., lidar return signal plus solar background – to levels manageable by the sensitive detectors. This approach was deemed acceptable because the operation at ground in daylight was required for engineering tests only.

With these critical design decisions made very early in the project, the design of what became the BOLIDE instrument was completed by late summer 2016. With the original launch date less than 1.5 years away, the implementation phase had to follow immediately. In particular, there was no time for testing the design on a breadboard or brassboard level.

A description of the PMC Turbo gondola and its power and communication systems can be found in Kjellstrand et al. (2020).

3 Description of the flight instrument
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The flight configuration of the BOLIDE instrument comprises three main components: (1) the pressure vessel housing the laser transmitter, receiver, electronics, main computer, and cooling system; (2) the receiving telescope; and (3) the radiator. A rendering of the instrument is shown in Fig. 1.

https://amt.copernicus.org/articles/13/5681/2020/amt-13-5681-2020-f01

Figure 1Computer rendering of the pressure vessel with the telescope attached (three side panels removed).

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3.1 Optical setup

Before going into details of the mechanical construction, let us first have a look at the optical setup depicted in Fig. 2. The laser is a frequency-doubled master oscillator power amplifier (MOPA) system built by Montfort Laser GmbH with 4.2 W average output power at 532 nm wavelength, 100 Hz pulse repetition frequency, and 5 ns pulse length. The laser uses thermoelectric coolers for heat removal and thermal stabilization and can thus be fully conductively cooled with no requirement for circulating coolant directly through the pump chambers. In the case of BOLIDE, the laser is mounted on an aluminum plate which serves as both structural member and heat sink. Glycol is pumped through channels embedded in the plate to remove waste heat. Residual 1064 nm light is separated by a dichroic mirror and subsequently dumped. A turning mirror mounted on a fast piezo-driven tip–tilt platform with 3.5 mrad angular range directs the remaining 532 nm beam to the first beam expander (). This beam expander is motorized for in-flight adjustment of the beam divergence. Further turning mirrors guide the beam to the second beam expander, which increases the beam diameter 2.5-fold to approximately 40 mm and reduces the beam divergence to 77 and 56 µrad for the fast and slow axis, respectively. The expanded beam exits the pressure vessel through a 102 mm diameter anti-reflective coated window. A final set of beam-turning mirrors relay the beam into the tube of the receiving telescope, where it is transmitted into the sky at a location 0.21 m offset from the optical axis of the receiving telescope. Piezo drives on the motorized mirror allow for coarse adjustments to the beam pointing, while the piezo-driven tip–tilt mirror is used to fine-tune the overlap between laser beam and FOV of the telescope.

https://amt.copernicus.org/articles/13/5681/2020/amt-13-5681-2020-f02

Figure 2Schematics of the optical system. APD: avalanche photodiode; BS: beam splitter; IF: interference filter; M: turning mirror; PMT: photomultiplier tube; SHG: second-harmonic generator. See text for details.

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The receiving telescope uses a 0.5 m diameter f∕2.4 quartz mirror with 38 mm edge thickness supported by a three-armed mirror cell. Light collected by the mirror is coupled directly into an Optran UV fiber (200 µm core diameter, NA 0.22) mounted in the focal plane, and a motorized spring-loaded vertical translation stage allows for fine tuning of the telescope focus in flight. The resulting FOV of the telescope as determined by the diameter of the fiber core is 165 µrad. The spot size of the mirror (15 µm) is much smaller than the facet of the fiber; thus coupling losses are negligible except for 8 % losses due to uncoated fiber ends. In order to minimize focus changes related to variations in temperature, the central spider holding the fiber mount is supported by a three-legged truss made of carbon fiber tubes.

The optical fiber enters the lidar pressure vessel through a vacuum feed-through and terminates in front of a mechanical chopper rotating at 100 rotations per second synchronized to laser firing times. With three 60 long slits in the chopper blade, the resulting chopping frequency is 300 Hz. The chopper blocks the intense signal originating from scattering of the laser beam in the vicinity of the receiving telescope, thus preventing the detectors from overloading. A collimation lens collimates the beam before passing through a filter wheel loaded with neutral-density filters with the exception of one clear position. The filters are used only during ground tests and allow for sufficient attenuation of the solar background for operation of the detectors in daylight. In flight, the clear position is used exclusively. Finally, as shown in Fig. 2, the collimated beam is split into three beams which are directed to individual detectors: two avalanche photodiodes operated in Geiger mode (APD1 and APD2: Excelitas SPCM-ARQH-16) and a photomultiplier tube (PMT: Hamamatsu H12386-210). While the PMC backscatter signal can be handled by a single detector, we chose to add two additional detectors to cover the larger dynamic range of the Rayleigh backscatter signal originating in the lower atmosphere closer to the gondola. The splitting ratio between the three channels is approximately 90 : 9 : 1, with 90 % of the light reaching the upper detector APD1. Both avalanche photodiodes (APD1 and APD2) are gated such that peak photon-counting rates remain below 7 MHz in order to limit signal-induced noise which results from significant heating of the silicon chip. Narrowband interference filters in front of the detectors reduce the solar background and minimize cross-talk between detectors. The filters used are 0.3 nm bandwidth (full width at half maximum) and 70 % peak transmission (IF1), 0.8 nm bandwidth and 81 % peak transmission (IF2), and 1 nm bandwidth and 50 % peak transmission (IF3). The electrical pulses coming from the detectors are time-stamped with 800 ps precision, corresponding to 0.12 m range resolution using a three-channel MCS6A multiscaler from FastCOMTec GmbH.

3.2 Mechanical setup

In order to keep the costs of the BOLIDE instrument low, the decision was made to use off-the-shelf components wherever possible. This included the use of non-vacuum compatible components. Hence, the instrument was to be housed in a pressure vessel designed to withstand 1 bar differential pressure when sealed on the ground. The vessel is a two-piece aluminum structure with a welded, cube-shaped lower half of size 0.44 × 0.44 × 0.57 m3 and a machined lid. The lower part comprises 5 mm thick plates, a 10 mm thick flange, and welded-on straps which represent the structural interface to the balloon gondola. The lid contains the optical windows, feed-throughs for the optical fiber, coolant lines, and electrical cables, as well as a relief valve for pressure equalization. The lid and lower part are held together by 64 bolts and are sealed off using a single O-ring.

The internal parts of BOLIDE are distributed over five shelves mounted on a rack which is bolted to the lid (see Fig. 3). Having a firm connection between the rack and lid rather than between the rack and bottom half considerably simplifies the integration, as all optical, electrical, and fluid connections run through the lid. The shelves are stacked during integration from bottom to top and comprise the following sections: the cooling section, the high-speed photon counter, the laser mounted on the cooling plate, the receiver, and the electronics section. The cooling section houses a welded glycol coolant tank with 6 L volume; the coolant pump; and DC-to-DC converters for the laser, pump, and 12 V main bus. All components are mounted on a common aluminum plate which also serves as the bottom of the glycol tank and thus allows for good conduction of waste heat into the coolant. A heat sink and fan assembly which is thermally bonded to one of the walls of the tank removes waste heat from the air inside the pressure vessel by forced convection.

https://amt.copernicus.org/articles/13/5681/2020/amt-13-5681-2020-f03

Figure 3The pressurized section containing the lidar receiver, laser, and electronics. This picture was taken during integration with the bottom half of the pressure vessel removed.

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The second shelf carries the photon-counting electronics whose heat sink is thermally connected to the lower face of the laser-cooling plate. Next follows the laser with the second beam expander protruding vertically into the receiver section above. The receiver shelf carries the optical assembly of the receiver, including chopper, filter wheel, and detectors. It also carries the mount for the infrared airglow camera contributed by Utah State University. The electronics shelf carries electronics modules on both sides and serves also as a heat sink for the devices. The main components are the main computer, the field-programmable gate array (FPGA) board, piezo drivers, microcontrollers, power switches, and signal converters.

3.3 Liquid cooling system

The active cooling system uses a single glycol cooling loop to remove waste heat generated inside the pressure vessel. A rotary vane pump draws coolant (brand name Tyfocor Art LS) from the glycol tank, which acts as both reservoir and accumulator and is located at the lowermost shelf. The liquid then passes through the laser-cooling plate and the external radiator, where the waste heat is finally radiated into space, before it is returned to the tank at a lower temperature. The one-sided radiator has an active surface of 1.6 m2 and is capable of rejecting 550 W at 18 C inlet temperature and flow rate of 6 L min−1. Electrical bias heaters mounted at the back side of the radiator are used to control the temperature of the glycol at the outlet and thus inside the glycol tank. The operating temperature of the cooling loop is constrained to 16–22 C, which is the temperature range in which the laser system was tested. In order to keep the heat load on the radiator and thus the glycol temperature constant, replacement heaters located at the bottom of the glycol tank are activated when the laser is not in use. A detailed description of the thermal control system and analysis is presented in Baturkin et al. (2020).

https://amt.copernicus.org/articles/13/5681/2020/amt-13-5681-2020-f04

Figure 4The PMC Turbo gondola during launch preparations on 6 July 2018.

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3.4 Power system

The BOLIDE instrument is supplied with unregulated 28 VDC primary power from the battery bus of the gondola. The primary power is internally distributed to a 12 V DC-to-DC converter, which supplies the main instrument bus, and two 24 V DC-to-DC converter providing power to the laser and the coolant pump. Moreover, the laser replacement heater and radiator bias heaters are connected to the primary power via computer-controlled relays. In order to maintain a constant heat load on the cooling system, the laser replacement heater, which dissipates the same amount of electrical power as the laser, is switched on whenever the laser is switched off. The radiator bias heaters are located on the radiator and are used to control the temperature of the coolant at the outlet of the radiator by biasing the temperature of the radiator surface.

All other electrical equipment is supplied from the 12 V instrument bus or a 5 V secondary bus. Each electrical system can be isolated through a series of power switches which are controlled by the main computer. Voltage and current sensors in the four secondary busses and the primary bus allow monitoring of the power consumption and voltage levels. The information is used by fault protection algorithms implemented in the main computer to assess the health of the instrument, as well as to protect the instrument from undervoltage conditions and overloads. All power switches are configured as normally open, causing the switches to open and automatically isolate downstream equipment should an undervoltage condition occur. The only exception is the switch through which power is supplied to the main computer. This switch is controlled by a dedicated microcontroller and is configured as normally closed in order to allow for automatic power-up of the computer when power is supplied to the instrument. A watchdog timer implemented in the microcontroller cycles the power switch should the software running on the main computer lock up and fail to send a heartbeat signal to the microcontroller. Power cycling causes an automatic restart of the computer followed by entry into safe mode with all equipment not critical for survival of the instrument being powered off.

3.5 Computer systems

BOLIDE uses a single-board computer (SBC) produced by Advantech as the main computer. The MIO-5271Z-4GA9A1E SBC features an Intel i5-4300U CPU running at 1.9 GHz clock rate and 4 GB RAM, and consumes about 15 W of power under load. The SBC's two Ethernet ports are connected to the local area network of the gondola for air-to-ground communication and to the embedded controller/FPGA, which acts primarily as a multiplexer/demultiplexer for the various sensors, actuators, and power switches used in BOLIDE. The photon counter and cameras are connected to the computer via USB, while the laser controller and microcontroller use RS-232 interfaces. For program and data storage, the computer uses three redundant solid-state disks with a total capacity of 4 TB. The computer runs Linux as its operating system and custom application software written in C/C++.

The embedded controller/FPGA board is a sbRIO-9637 with a 667 MHz dual-core processor and a Zynq-720 FPGA from National Instruments. The primary intended use of the FPGA is the implementation of interfaces to sensor and control busses and the implementation of the synchronization logic and timing loops which control all time-critical tasks, for example triggering of laser pulses, start of data acquisition, and gating of detectors. Furthermore, several safety features with regard to operation of the laser are implemented in the FPGA. These include the automatic shutdown of the laser in the case of an out-of-bounds attitude of the gondola or out-of-bounds altitude, or when the command loss timer expires.

3.6 Flight data system and command & control system

The flight data system (FDS) comprises software running on both the main computer and the embedded controller/FPGA. Its main purpose is to collect science data from the photon counter and cameras, as well as telemetry from various subsystems, and to format the data for transmission to ground and for onboard storage. Two engineering and seven mixed science and engineering data formats which require downlink bit rates ranging between 1.2 and 26 kbit s−1 are implemented in the FDS. A basic science frame containing a full photon count profile of the high-rate channel (detector APD1; see Fig. 2) with 100 m range resolution is included in all mixed formats and sent to ground every 2 s. These high-priority science data are interleaved with basic engineering data and a variable number of lower-priority sub-frames filled with higher-resolution science data. All frames are compressed using zlib before being queued for downlink. While the high-priority frames are retrieved from the queue and sent to ground immediately, the low-priority frames remain in the queue until a frame fits into the downlink data stream whose capacity is defined by the selected bit rate. This scheme maximizes the amount of science data reaching the ground while taking into account the variable efficiency of data compression.

The command & control system (CCS) receives commands from the ground, validates the commands, and stores the commands in a sequencer table. A software loop scans the table 10 times per second for commands which are tagged for execution. These commands are then removed from the table and forwarded to the appropriate subsystems.

Commands are sent from the ground in command loads, which are lists of commands encapsulated in special headers and footers. The latter are used by the CCS for validation of a command load and to verify its integrity via check sums. Commands can be either real-time commands which are executed as soon as they are received by the CCS or time-tagged commands which are scheduled by the sequencer for execution at later times. With time-tagged commands, execution times can be specified as absolute times – i.e., relative to the epoch of the main clock – or as time offsets relative to the execution time of a previous command. This sequencing capability allows for a great deal of flexibility in controlling the instrument even when no satellite link is available for real-time commanding. One particularly critical part of the mission without real-time commanding capability is the descent phase when the thermal control system needs to be reconfigured as a result of the rapidly changing environmental conditions.

4 Predicted and in-flight performance
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The performance of the lidar instrument was predicted by solving the lidar equation for the given set of instrument parameters (see Table 2). In order to model the solar background picked up by the instrument, sky radiances were calculated using the libRadtran software package for radiative transfer calculations (Emde et al.2016) and converted to photon-counting rates. These background rates were then integrated, taking into account the length of the lidar range gates and number of laser pulses, and added to the simulated lidar profile. A detailed description of the simulation and underlying equations is presented in the Appendix.

Table 2Instrument parameters used in the performance simulations.

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Figure 5 shows background photon-counting rates for three different solar elevation angles as a function of altitude. Forty-five degrees represents the maximum solar elevation, which occurs at solar noon on 24 December at 68 S. Because long-duration balloons launched from McMurdo remain generally southward of 68 S and solar elevation angles at solar noon are lower before and after 24 December, the 45 trace in Fig. 5 can be seen as the worst-case scenario for the Rayleigh background. However, it is important to note that the simulation includes a telescope with an unobstructed view of the sky, whereas in reality the spider of the telescope is within the telescope FOV and photons scattered off the spider vanes enhance the background counting rates. How much the spider contributes to the total background depends on several factors (e.g., exact geometry, surface reflectivity, effective sky brightness) which are difficult to estimate. We will discuss these factors in Sect. 5.

https://amt.copernicus.org/articles/13/5681/2020/amt-13-5681-2020-f05

Figure 5Simulated background photon-counting rates for the 83 µrad (gray) and 165 µrad (black) telescope FOV and 2, 20, and 45 solar elevation angles. The 165 µrad FOV was eventually used during the mission.

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https://amt.copernicus.org/articles/13/5681/2020/amt-13-5681-2020-f06

Figure 6GPS altitude of the gondola (a) and measured and simulated lidar background (b) between the evening of 10 July and morning of 11 July 2018. The simulation (red line) includes the actual altitudes and solar elevation angles.

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The 2 trace in Fig. 5 marks the Rayleigh background for solar midnight at 70 S on 1 December. This is about the earliest launch opportunity for a long-duration balloon, and later launches result in larger minimum solar elevation angles and hence a larger background. Thus, the area between the 2 and 45 lines characterizes the maximum potential variation of the Rayleigh background during the originally planned Antarctic mission. The flight track of the eventually executed mission remained within the same latitude band albeit in the Northern Hemisphere, and thus the same estimates apply. Considering floating altitudes between 35 and 39.5 km, the expected Rayleigh background lies between 50 and 180 kHz. It is worth mentioning here that the floating altitude of zero-pressure balloons varies by 3–4 km in response to solar heating; i.e., the balloon rises in the morning and descends in the evening (see Fig. 6). On the one hand greater heights result in lower background rates as shown in Fig. 5, and on the other hand larger solar elevation angles cause greater sky brightness and hence larger background rates. Because the variations in altitude and in solar elevation angle are in phase, the two effects roughly cancel each other and the simulated Rayleigh background (red line in Fig. 6) is rather constant at approximately 90 kHz. However, actual measurements of the total background rate are 2–3 times larger and follow the trend of the solar elevation.

https://amt.copernicus.org/articles/13/5681/2020/amt-13-5681-2020-f07

Figure 7(a, b) Measured (black) and simulated (colored) photon count profiles for a 30 s integration period on 11 July 2018 at 04:07 UTC. The peak βPMC in panel (a) is 42×10-10m-1sr-1. Panel (b) shows simulated profiles with a peak βPMC of 2×10-10m-1sr-1 for the configuration 165 µrad FOV and high background (red), 165 µrad FOV with Rayleigh background only (brown), 83 µrad FOV with high background (purple), and 83 µrad FOV with Rayleigh background only (blue). (c) PMC backscatter βPMC in units of 1×10-10m-1sr-1 shown for a 4 h period centered around the profile in panel (a).

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With all known factors taken into account, our simulations yielded a simulated lidar return signal which is larger than what our instrument detected in flight. However, when the simulated signal is decreased by 38 %, simulation and actual measurements are in good agreement. This led us to conclude that there are unknown signal losses somewhere in the optical path, most likely caused by misalignment of the last lens in front of the detector (see Sect. 5). On the other hand, the comparison between simulated and measured background revealed that our simulation is underestimating the background by 100 to 300 % depending on time of day. Figure 7 shows measured and simulated photon count profiles for a 30 s integration period on 11 July at 04:07 UTC. In order for the simulation to reproduce the measured profile, the transmission of the receiver was artificially reduced by 38 % and the background increased by 280 %.

In order to assess the detection threshold of the BOLIDE instrument, we calculated the backscatter ratio and the volume backscatter coefficient of the PMC (βPMC) using the NRLMSISE-00 density profile of the atmosphere for July and 69 N as a reference density profile (Picone et al.2002). The PMC signal in Fig. 7a originates from a rather bright cloud with a peak βPMC of 42×10-10m-1sr-1. We used the profile of βPMC scaled to a peak value of 2×10-10m-1sr-1 as a reference profile for the following simulations shown in Fig. 7b: the red profile represents the configuration as flown with a telescope FOV of 165 µrad and a background which is 2.8 times the Rayleigh background. For the brown profile we assume that the additional background can be avoided through better shielding of the telescope; i.e., we consider only the Rayleigh background. This is a pathological case in the sense that the spider which is located within the FOV of the telescope will always contribute some additional background. Finally, the background can be lowered further if we reduce the telescope FOV to 83 µrad by using a smaller optical fiber. The impact of this smaller FOV is demonstrated by the last two curves in Fig. 7b: for the purple profile we again assume a background which is 2.8 times the Rayleigh background and thus represents a conservative estimate assuming that the shielding of the telescope cannot be significantly improved. In contrast, if the telescope can be perfectly shielded, we end up with the blue profile. The latter represents the optimum performance and technological limit of the BOLIDE instrument. Following Kaifler et al. (2013) we define a PMC as detectable if the PMC signal with the background removed is larger than 2.5 times the measurement uncertainty (1σ error). We find detection thresholds of 0.58, 0.38, 0.33, and 0.19 in units of 10−10m-1sr-1 for the four simulated profiles shown in Fig. 7b. The first value (0.58) applies to the flight configuration and thus represents the detection threshold in the acquired data. In total, the instrument recorded backscatter profiles of PMCs (β>2×10-10m-1sr-1) during 70 h out of the  5.9 d flight.

Temperature profiles were retrieved by hydrostatic integration of photon count profiles below the PMC layer (Hauchecorne and Chanin1980). Here, the excessive background noise becomes strongly noticeable and effectively limits the resolution of retrieved temperatures to 1.3 km in the vertical and 20 min in time. Examples of BOLIDE temperature data are shown in Fritts et al. (2019). The retrieval of temperature profiles above the PMC layer as demonstrated in Kaifler et al. (2018) is not possible due to the high background and the resulting poor signal-to-noise ratio above the layer.

5 Discussion
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As demonstrated in Fig. 7 and in more detail in the overview paper by Fritts et al. (2019) and the study by Fritts et al. (2020), lidar measurements acquired by the BOLIDE instrument during the PMC Turbo mission yielded high-resolution backscatter profiles of PMC. All requirements (see Table 1) were met, and the performance surpassed that of the largest ground-based lidar systems. Kaifler et al. (2018) achieved a higher peak sensitivity of 0.1×10-10m-1sr-1 with their ground-based system, but their integration time of 120 s is 4 times larger compared to BOLIDE, and measurements were obtained for a few hours in darkness only, while BOLIDE acquired continuous measurements with approximately constant sensitivity for days. We note that Kaifler et al. (2013) and Ridder et al. (2017) present PMC backscatter profiles at higher resolution of 30 s and 40 m, but no information on the detection threshold is given. A subset of the data in Kaifler et al. (2013) is shown at a resolution of 0.33 s× 25 m. We want to highlight that BOLIDE data can be processed at even higher resolutions, albeit at the cost of a higher detection threshold as compared to the standard resolution of 30 s× 100 m. Examples with a resolution of 10 s× 20 m are presented in Fritts et al. (2020). Figure 8 demonstrates the high-resolution capabilities of the BOLIDE instrument. While Fig. 8a shows a 10 min section at 10 s× 100 m resolution, the temporal and vertical resolution are increased by a factor of 33 and 4, respectively, in Fig. 8b. At this high resolution the fine structure of the PMC layer with multiple sharply bounded sublayers with a thickness of a few tens of meters becomes visible. Even higher resolutions up to 0.1 s and 5 m are possible and may be used where PMCs are bright, i.e., where the signal is large.

https://amt.copernicus.org/articles/13/5681/2020/amt-13-5681-2020-f08

Figure 8Photon counts of a 10 min section of the data shown in Fig. 7c with (a) 10 s× 100 m resolution and (b) 0.3 s× 25 m resolution.

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https://amt.copernicus.org/articles/13/5681/2020/amt-13-5681-2020-f09

Figure 9Normal (a) and overexposed (b) image of the upper part of the telescope taken by the side-viewing onboard camera. Panel (c), taken by an upward-looking engineering camera inside the pressure vessel, shows the balloon above the gondola.

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The comparison of our high-resolution data (Fig. 8b) with Fig. 9 in Kaifler et al. (2013) reveals that maximum photon counts detected by BOLIDE are a factor of  5 larger. We note that raw photon counts are uncalibrated data and depend on PMC brightness; hence a direct comparison of the performance of the respective instruments is not possible based on just photon counts.

When comparing the actual performance to pre-flight predictions, we found two major discrepancies: (1) the detected lidar signal was 38 % lower and (2) the background was a factor of 2–4 higher. The latter number is a rough estimate because the answer to the question of how much additional background BOLIDE detected depends ultimately on where the unexpected signal loss occurred. Based on post-flight tests, the most likely cause of the signal loss is a misalignment between the last lens of the optical system and the APD detector (see Fig. 2). This particular lens has a focal length of 8 mm and, for optimal detection efficiency, has to be precisely aligned to the optical axis of the detector. Because the active area of the APD is only 180 µm in diameter, any even small misalignment leads to significant losses which affect the lidar signal and the background in exactly the same way. If, however, the detected signal loss had been caused by incomplete overlap between the telescope FOV and the laser beam, for example as a result of a much larger beam divergence, then only the lidar signal would have been affected. Thus, in this scenario the relative increase in background relative to pre-flight predictions would be lower as compared to the previous case, where lidar signal and background are affected in the same way. Due to this uncertainty, we cannot put narrower constraints on the background.

The unexpectedly high background was identified as a potential problem in the early design phase of BOLIDE. As evident from Fig. 9c, the balloon above the gondola acts as a bright and diffuse light source which illuminates the gondola and the telescope. Because of the height requirement (Table 1), there was no way to extend the baffle of the telescope and shield the spider vanes from light scattered off the balloon. Indirect illumination where the light scatters off the inside of the telescope tube first and then hits the underside of the spider vane is also possible, but was not investigated during the design phase due to time and financial constraints as well as the lack of a clear understanding of the optical properties of the balloon. Images taken during the flight documented that the spider vanes are indeed significantly illuminated by the balloon. While the inside of the telescope appears pitch black against bright sunlit tropospheric clouds (Fig. 9a), the overexposed image reveals the spider vanes and the focusing assembly inside the telescope (Fig. 9b). That is only possible if the inside of the telescope is illuminated from above. Rayleigh scattering in the atmosphere above the gondola can be ruled out as a major source because the radiance as seen from the gondola is roughly constant over a period of 24 h, whereas the measured background shows a clear dependence on the solar elevation angle (see Fig. 6). Hence, the balloon must be the dominating light source.

There are two obvious solutions to the background problem: the addition of a baffle to prevent stray light from entering the telescope and the use of an off-axis telescope. As noted above, the former was not possible for the PMC Turbo mission because of height constraints but can be accommodated in a future mission with a redesigned gondola. The use of an off-axis telescope is an elegant but costly solution. Because such a telescope does not require a spider, there is no obstruction within the FOV of the telescope and thus no possibility for stray light entering the optical path except for scattering at the mirror surface. Reducing the telescope FOV from 165 to 83 µrad helps in both ways as it not only decreases the additional background due to the smaller acceptance angle but also reduces the Rayleigh background (see Fig. 7). A FOV of 83 µrad is technically possible with the BOLIDE system, though in this case the laser beam nearly completely fills the telescope FOV with little margin. Since we had no previous experience with operating a lidar on a balloon, we were not sure about the mechanical and thermal stability of the laser–telescope assembly and the vibration environment at floating altitude. Therefore, we opted for a conservative approach and used the larger FOV, which tolerates larger excursions of up to  40 µrad off the nominal beam position without degradation of the lidar return signal. Tests carried out during the flight suggested a low-vibration environment and very stable beam pointing. Hence, in future flights of the BOLIDE instrument we plan to use the small FOV. As evident from the simulations shown in Fig. 7, the small FOV in combination with better shielding or an off-axis telescope will push the background to a value below the Rayleigh scattering at the PMC altitude. In that case the PMC detection threshold will be determined by the Rayleigh scattering rather than the background, and no further improvements are possible unless the laser power or the telescope aperture (or both) is increased.

From an operational point of view the instrument performed well throughout the flight. No degradation of the optics was observed and signal levels remained constant. The flight software worked as expected with one exception: a bug in the data acquisition software of the lidar caused the data acquisition to stop after approximately 12 h, and the only way to exit this condition was a manual restart. Although the capability to patch the flight software in flight was built into the software, we did not make use of it because the stop times were predictable and restarts could be initiated via real-time or time-tagged commands. Later, the inspection of the source code revealed that the bug would have been caught before the flight with longer integrated testing of the hard- and software, as pre-flight testing had been limited to continuous runs of about 8 h. The downlink of real-time science data proved to be valuable for the assessment of science conditions and PMC brightness and, in particular during the early hours of the flight, served as guidance for the imaging experiments. We also made frequent use of the commanding capability to adjust settings and thus optimize the performance of the instrument.

6 Conclusions
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As noted above, the BOLIDE experiment turned out to be highly successful during its maiden 6 d long flight in July 2018. It met all design requirements and provided science data of PMCs with better quality (higher resolution and lower detection threshold) than continuously operating ground-based lidar experiments. The high-resolution (0.3 s× 25 m) capability of the data processor was demonstrated and revealed sharply bounded PMC sublayers of less than 100 m thickness.

The comparison of in-flight performance and predicted performance revealed that the instrument suffered from excessive background noise caused by light scattered off the balloon entering the optical path. Two obvious solutions for this problem are the addition of a baffle to prevent stray light from entering the telescope and the use of an off-axis telescope.

BOLIDE also demonstrated that it is possible for a small team of dedicated scientists and engineers to design, develop, and build the flight hardware within a short period of about 2 years. In addition to providing science data, the primary goal of the BOLIDE project was to demonstrate for the first time the operation of a high-power lidar on board a balloon platform. In this regard the authors hope that the successful operation of BOLIDE paves the way for more capable and more ambitious future balloon lidar experiments. An obvious candidate is a compact iron resonance lidar for measuring high-altitude winds and temperatures (Kaifler et al.2017).

Appendix A: Equations used in the simulation
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The Rayleigh signal per laser pulse at altitude z integrated over the height of an altitude bin Δz is given by

(A1)SRayz=Δzρ(z)σ180(λ)Az-z2N,

where ρ(z) is the number density taken from the NRLMSISE-00 model (Picone et al.2002), σ180(λ) the Rayleigh backscatter cross section, and A(z-z)-2 the solid angle formed by the aperture of the telescope with area A and distance z-z. Note that z describes the altitude of the telescope, i.e., the floating altitude of the gondola. The number of photons emitted per laser pulse is expressed as

(A2)N=Eλhc,

with the pulse energy E, Plank's constant h, and the speed of light c. For the wavelength λ of our laser we used the value 532.32 nm (vacuum wavelength). The backscatter cross section is computed via

(A3)σ180(λ)=14π32σ(λ).

The factor 3∕2 originates from the Rayleigh phase function for the scattering angle of 180, and the total scattering cross section σ=5.16×10-31m−2 is calculated from the equations given in Bucholtz (1995).

We simulated the solar Rayleigh background based on sky radiances calculated for given altitudes z and the looking direction anti-Sun 28 off zenith using the libRadtran software package for radiative transfer calculations (Emde et al.2016). The radiances Le,Ω were converted to received power as

(A4)Pz=Le,ΩzAΩB,

where Ω=π(0.5FOV)2 is the solid angle of the telescope with the FOV. B is the transmission bandwidth of the interference filter in the receiver (see Fig. 2). In general one would have to integrate the product of wavelength-dependent radiance and filter transmission over the full spectrum to obtain the received power. Because there are no Frauenhofer lines within the passband of our 0.3 nm wide filter, for simplicity we assumed a constant radiance and replaced the transmission function with a corresponding rectangular function with the same area as the transmission function integrated over the full spectrum. In our case we obtained B=0.250nm. In a next step, the Rayleigh background photon rate can be expressed in analogy to Eq. (A2) as

(A5)nBG=P(z)λhc.

After multiplying by τ=2Δzc-1, which is the period of a range gate, the resulting background photons per range gate can be added to the Rayleigh signal to form the total photon profile. Multiplication with the number of laser pulses per integration period, Δtfrep, yields the received photon count profile

(A6)S(z)=ηΔtfrepSRay(z)+τnBG.

Here Δt is the integration period and frep the pulse repetition frequency of the laser. The prefactor η in Eq. (A6) is the efficiency of the lidar system and is computed as the product of all efficiencies and transmission coefficients listed in Table 2. Taking into account the additional 38 % signal loss in the receiver (see Sect. 4), we used η=0.191 as the final value.

The photon count profile described by Eq. (A6) is valid for a perfect noise-free system. In order to simulate the shot noise of the photon-counting process, in a final step we replaced each count value of S(r) – i.e., the number of detected photons for a given range gate – with a random number drawn from a Poisson distribution where the expected value of the distribution equals the original count value.

Data availability
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Data availability. 

Data are available on the HALO database at https://halo-db.pa.op.dlr.de/mission/112 (German Aerospace Center2020).

Author contributions
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Author contributions. 

BK came up with the idea for the BOLIDE instrument, built the receiver, managed the project, and wrote the manuscript. DR designed the pressure vessel and telescope. CB built the laser transmitter system. NK wrote the software for the instrument and performed data analysis. VB designed the thermal control system. PR designed and built the electronics

Competing interests
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Competing interests. 

The authors declare that they have no conflict of interest.

Acknowledgements
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Acknowledgements. 

Development of the BOLIDE instrument was supported by DLR. The gondola was funded partly by NASA and DLR and was built by the PMC Turbo team with support from NASA. The authors thank David C. Fritts and NASA for the flight opportunity, Markus Rapp for acquiring funding, and the staff of the Columbia Scientific Balloon Facility for their excellent support during preparation and execution of the mission.

Financial support
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Financial support. 

The instrument and research was supported by DLR internal funding. The balloon mission was supported by NASA.

The article processing charges for this open-access
publication were covered by a Research
Centre of the Helmholtz Association.

Review statement
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Review statement. 

This paper was edited by Jorge Luis Chau and reviewed by three anonymous referees.

References
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Short summary
The Balloon Lidar Experiment was the first lidar dedicated to measurements in the mesosphere flown on a balloon. During a 6 d flight, it made high-resolution observations of polar mesospheric clouds which form at high latitudes during summer at ~ 83 km altitude and are the highest clouds in Earth's atmosphere. We describe the instrument and assess its performance. We could detect fainter clouds with higher resolution than what is possible with ground-based instruments.
The Balloon Lidar Experiment was the first lidar dedicated to measurements in the mesosphere...
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