instrumentation

HAO flew observers to MLSO to observe the Sun during the solar eclipse

whawkins — Tue, 12 Mar 2024 17:35:55 +0000

HAO flew observers to MLSO to observe the Sun during the solar eclipse whawkins Tue, 03/12/2024 - 11:35

Author:

whawkins

Mar 12, 2024

Helicopter flying in batteries and solar panels to MLSO located at 11,200 feet on Mauna Loa. The observatory domes are visible at left.

On April 8, 2024, the day of the total solar eclipse, HAO observers Ben Berkey (site manager) and Lisa Perez-Gonzalez flew by helicopter (the road is still closed due to the volcanic eruption of 2022) to the Mauna Loa Solar Observatory (MLSO) located at 11,200 feet on the north face of Mauna Loa to observe the Sun’s corona using the MLSO coronagraphs. During an eclipse the moon blocks out the bright disk of the Sun making the faint pearly corona visible. Coronagraphs are instruments that create ‘artificial’ eclipse images, using a disk inside the telescope to block the bright disk of the Sun. Unfortunately, clouds prevented observations on April 8, but Ben and Lisa were able to return on April 9 to capture beautiful observations of the corona with both coronagraphs.

The Corona on April 9, 2024

An image of the corona from the MLSO K-Coronagraph (K-Cor) in ‘white light’, similar to what is visible with the naked eye.

The MLSO UCoMP coronagraph image of the iron emission line of Fe XIII at a wavelength of 1074.7 nm. This emission line captures plasma with temperatures of ~1.6 million degrees. That is hot enough to strip 12 of the electrons from these iron atoms.

About 4 hours of coronal observations were acquired on April 9 with K-Cor and UCoMP. There are different types of data products available online from UCoMP and from K-Cor.

The Solar Cycle

Royal Observatory of Belgium

The April 8, 2024 eclipse occurred very close to solar maximum activity, when the corona tends to be at its brightest. This plot above shows the ’11-year sunspot cycle’. The Sun goes through peaks and lulls in solar activity that last ~11 years. The plot shows the rise and fall in the number of sunspots. Sunspots are regions of very strong magnetic field. Solar activity, such as flares and explosive events known as coronal mass ejections (CMEs), derive their energy from the Sun’s magnetic field. Solar activity rises, on average, with the number of sunspots.

Don Kolinski

The April 8, 2024 eclipse showed a beautiful ‘solar maximum’ corona, with bright structures all around the Sun. Cool, dense structures known as prominences were also visible during the eclipse. This is a photo of the April 8th eclipse by HAO’s Don Kolinski. The reddish-colored structures seen around the corona are prominences. These are often seen erupting as part of a CME. The best chance to see a prominence during an eclipse is at solar maximum.

By contrast, the solar corona during solar minimum activity looks very different, as shown in this image, taken by the MLSO K-Cor instrument in 2019 when sunspots were near zero. There are very few bright prominences present at solar minimum.

Scientists are using the April 2024 observations of the corona from MLSO, eclipse experiments, and other ground- and space-based data to study the coronal magnetic field and plasma conditions during solar maximum.

For information on the MLSO observing plan and other eclipse-day experiments and modeling efforts please see the WHPI 2024 eclipse campaign.

MLSO UCoMP Science Data Now Available

kolinski — Tue, 19 Dec 2023 20:31:47 +0000

MLSO UCoMP Science Data Now Available kolinski Tue, 12/19/2023 - 13:31

Author:

kolinski

Dec 19, 2023

The Mauna Loa Solar Observatory Upgraded Coronal Multi-Channel Polarimeter (UCoMP) coronagraph science data (version 1.0.1) have now been released to the community via the Mauna Loa web page.

Sample of UCoMP data on the MLSO website.

These data cover the period from July 18, 2021 through Nov 9, 2022. UCoMP observes the solar corona from 1.04 to ~2 solar radii in 9 coronal emission lines. Data have been released for 5 coronal emission lines: FeXIII 1074.7 and 1079.8 nm; FeXI 789.4 nm; FeX 637.4 nm; and FeXV 706.2 nm. Science products are in fits format and include: Level 1 observations of Stokes I, Q, U, and V at multiple wavelengths across each emission line; Level 2 products: Intensity [center wavelength, enhanced and peak]; line-of-sight Doppler velocity; FWHM Line Width; weighted average Stokes I, Q, U, V and linear polarization; plane-of-sky magnetic field azimuth and radial azimuth; and a noise mask. Quicklook images and movies are also provided.

The UCoMP Data User Guide is provided with every fits tar download and quicklook zip download. Please see the user guide for more information.

This is the first release of the data and some problems remain. The most significant are stray light, wavelength tuning drift and image alignment. The stray light and wavelength drift impact the line width and Doppler images. We are working to solve these issues for the next release in 2024. The guide includes the link to the GitHub system where you can read details about all UCoMP issues.

Please report any problems or questions about UCoMP data to mlso_data_requests@ucar.edu

A Spectroscopic Survey of Infrared 1–4 μm Spectra in Regions of Prominent Solar Coronal Emission Lines of Fe XIII, Si X, and Si IX

kolinski — Mon, 11 Jul 2022 18:57:40 +0000

A Spectroscopic Survey of Infrared 1–4 μm Spectra in Regions of Prominent Solar Coronal Emission Lines of Fe XIII, Si X, and Si IX kolinski Mon, 07/11/2022 - 12:57

Publication: The Astrophysical Journal; Authors: Aatiya Ali, Alin Razvan Paraschiv, Kevin Reardon, and Philip Judge

Author:

kolinski

Jul 11, 2022

The infrared solar spectrum contains a wealth of physical data about the Sun and is being explored using modern detectors and technology with new ground-based solar telescopes. One such instrument will be the ground-based Cryogenic Near-IR Spectro-Polarimeter of the Daniel K. Inouye Solar Telescope (DKIST), which will be capable of sensitive imaging of the faint infrared solar coronal spectra with full Stokes polarization states. Highly ionized emission lines have been observed in galaxies and the solar corona. Quantifying the accuracy of spectral inversion procedures requires a precise spectroscopic calibration of observations. A careful interpretation of the spectra around prominent magnetic dipole lines is essential for deriving physical parameters and particularly for quantifying the off-limb solar coronal observations from DKIST. In this work, we aim to provide an analysis of the spectral regions around the infrared coronal emission lines of Fe xiii 1074.68 nm, Fe xiii 1079.79 nm, Si x 1430.10 nm, and Si ix 3934.34 nm, aligning with the goal of identifying solar photospheric and telluric lines that will help facilitate production of reliable inversions and data products from four sets of solar coronal observations.

Fe XIII 1074.68 nm emission over atmospheric absorption (normalized) in the He I Cryo-NIRSP wavelength range with all labeled candidate lines. The green curve represents the atmospheric spectra that are convolved with a Gaussian function correspondent to the Cryo-NIRSP 0"5 slit spectral resolution of 0.027 nm.

NSF Approves Funding for COSMO Next Stage

kolinski — Mon, 07 Mar 2022 17:30:25 +0000

NSF Approves Funding for COSMO Next Stage kolinski Mon, 03/07/2022 - 10:30

COSMO Site and Design Advancement Updates

kolinski — Mon, 07 Mar 2022 16:47:44 +0000

COSMO Site and Design Advancement Updates kolinski Mon, 03/07/2022 - 09:47

Author:

kolinski

Mar 7, 2022

Recent NSF Funding for COSMO Site and Design Advancement (COSADA)

Final Design of COSMO Large Coronagraph (LC)
Site Survey

Final Design of COSMO Large Coronagraph (LC)

The National Science Foundation (NSF) has provided funding for the final design of the COSMO Large Coronagraph (LC). At 1.5 meter aperture, the LC will be the world’s largest refractive telescope, and will enable observations of the global coronal magnetic fields. The LC will have a 1° field of view (FOV), observing out to 2 solar radii, i.e., 1 solar radius above the solar surface, at all heliolatitudes, using a Stokes polarimeter and a narrow-band electro-optically tuned birefringent filter. The very broad wavelength range of the LC extends from the optical to the near infrared, allowing it to observe structures over a wide range of coronal temperatures. The polarimetric measurements diagnose the strength and direction of the coronal magnetic field. The LC’s large aperture will finally allow circular polarization measurements over the entire corona--these measurements are sensitive to the coronal magnetic field strength in the direction of the Sun-Earth line through the Zeeman effect. The linear polarization from resonant scattering of photospheric radiation is then used to measure the direction of the magnetic field in the plane of sky, orthogonal to the Sun-Earth line, along with coronal wave measurements which diagnose the plane-of-sky magnetic field strength.

Unlike a spectrograph, the LC’s tunable filter allows simultaneous observations over the entire FOV, combining the strengths of simultaneous 2-D imaging and high-resolution spectroscopy into a single instrument. The 1° FOV allows the study of typical large-scale coronal structures and enables the LC to track the build up of magnetic energy in the corona leading to solar eruptions known as Coronal Mass Ejections (CMEs). The broad wavelength provides information on coronal plasma thermal structure, density and dynamical status using standard diagnostic techniques.

The LC final design is a 3-year proposal that will produce a final design of the telescope and mount and will include all reviews and construction cost estimates for all specified LC elements. In March of 2021, UCAR contracts released a Request for Proposal for companies to propose to design the COSMO LC. Five excellent proposals were received as a result of the RFP. After an extensive evaluation process, the project selected European Industrial Engineering to award the LC design contract in June of 2021. A contract was executed and work on the design commenced in September of 2021. Steady progress on the design has ensued, and the first major milestone, the Systems Requirements Review, is scheduled for the week of March 7-11, 2022.

COSMO Site Survey

Identifying a final site for the COSMO observatory is necessary for significant risk reduction and for determining construction costs. Sites in Hawaii are known to have good coronal skies but other sites have not been fully tested. The site survey includes data-mining to determine candidate sites, data analysis, and construction and deployment of site testing equipment to six sites.

Figure 1. Damon Burke and Steve Tomczyk of HAO, shown with the COSMO Phase I site survey equipment currently at the NCAR Marshall Field site just south of Boulder Colorado.

The site survey equipment will be deployed in two phases. The first phase of instruments will be deployed to six sites and include:

Sky Radiometers to measure Sun and sky radiance from 315 to 2200 nm, to determine aerosol and other atmospheric properties. These operate robotically and require no dome.
Weather Stations to record solar radiation, wind speed and direction, air temperature, humidity, precipitation, etc.

Phase I instrumentation is shown in Figure 1.

The second phase will deploy an array of solar scintillometers to the sites that meet COSMO requirements. The solar scintillometers measure variation of atmospheric turbulence with height. These measurements provide the height dependence of seeing that determine the height of the telescope above the ground, which is an important cost driver.

HAO purchased, and deployed all phase one equipment to the NCAR Marshall site just south of Boulder, as shown in Figure 1. The equipment is fully automated, operating nominally and will continue to acquire observations at Marshall until they are deployed to the six COSMO sites.

UCoMP Instrument Nearing Science Mission Phase

kolinski — Fri, 04 Mar 2022 16:39:13 +0000

UCoMP Instrument Nearing Science Mission Phase kolinski Fri, 03/04/2022 - 09:39

Author:

kolinski

Mar 4, 2022

The Upgraded Coronal Multi-Channel Polarimeter (UCoMP) coronagraph was deployed to Mauna Loa Solar Observatory in 2021. UCoMP observes the solar corona from 1.03 to 2 solar radii over a wide range of wavelengths, allowing scientists to explore the magnetic structure of the Sun’s corona over a wide range of plasma temperatures. UCoMP observations are needed to help understand the physical processes behind the formation of solar eruptions known as Coronal Mass Ejections (CMEs). UCoMP is nearing the end of its commissioning phase and will begin to provide science observations to the community in the spring of 2022. For more information, please see the UCoMP instrument page:

www2.hao.ucar.edu/mlso/instruments/upgraded-coronal-multi-channel-polarimeter

UCoMP Level 1 and Level 2 data products from the FeXIII emission line at 1074.7 nm.

MLSO Facility gets a new dome!

kolinski — Fri, 17 Dec 2021 16:38:05 +0000

MLSO Facility gets a new dome! kolinski Fri, 12/17/2021 - 09:38

Outreach and Observing at Mauna Loa in Hawaii

kolinski — Fri, 17 Dec 2021 16:18:52 +0000

Outreach and Observing at Mauna Loa in Hawaii kolinski Fri, 12/17/2021 - 09:18

Author:

kolinski

Dec 17, 2021

The domes of Mauna Loa Solar Observatory under rare cloudy skies (photo by Michael Thompson, NCAR Deputy Director, Mesa Lab, Boulder, CO).

Educational outreach is an important and rewarding part of an observer’s job at the Mauna Loa Solar Observatory (MLSO) site located on the flanks of Mauna Loa Mountain at an elevation of 3440 meters in the U.S. state of Hawai’i. MLSO is operated by the High Altitude Observatory (HAO), a division of the National Center for Atmospheric Research, which is located in Boulder, Colorado.

Allen Stueben, (center), giving tour to14 high school students from Namiki High school in Japan.

The MLSO staff gives tours to mountain visitors a couple times a month. These groups of visitors range from colleges in the solar to atmospheric sciences, members of the public and school groups. This year's highlights included 14 high school students from Namiki High school in Japan, HAO/NCAR directors, and a tour of about 30 people from the International Astronomy Teaching Summit conference that happened in Hilo this past summer.

MLSO staff also participate in various community outreach events organized by the local astronomy community. These events typically attract a few hundred visitors and give MLSO a chance to share recent activity at the observatory as well as explain solar phenomena. During the 2018 Astroday West Hawaii event, MLSO made the front page of the local paper with the display featured in the linked article and depicted in the photograph "Lisa Waters" below. (http://www.westhawaiitoday.com/2017/11/06/hawaii-news/astro-day-lifts-off/). This years Astroday focused on magnetic fields and effects on the sun (right up our alley). One of our hands on activities had kids try to find magnets hidden behind sun-spots with little compasses.

Ben Berkey (bearded, lower right) giving tour to 30 people from the International Astronomy Teaching Summit conference.

HAO employs two full-time observers (Ben Berkey and Allen Steuben), one 3/4 time (Lisa Waters), and one casual observer (Greg Rose) on the mountain. Working at high altitude is challenging and the road to the summit, called Mauna Loa Scenic Drive or Mauna Loa Observatory Road, is a roughly paved and narrow 17-mile drive that climbs at an average 4.98% grade. For most, the drive is a once in a life time trip, but for our intrepid MLSO team it is a weekly commute.

As Ben Berkey likes to say "the days are long but far between." He describes a day that begins at sea level (Hilo on the east coast) and well before sunrise. Then, in a race against time, he travels upward along a treacherous road gaining thousands of meters in elevation. With luck, over an hour into the drive, he will emerge above cloud level into a clear sky; the world begins to brighten. At this point it is still a half an hour of travel and additional thousands of meters to gain while winding through a stark landscape of barren mounds of a'a or lava. Upon arriving at the observatory "temple", devoted to the study and tracking of the sun, it is a sudden flurry of activity to begin the day's tasks. Sleeping computers must be awakened and inspected to ensure their readiness for the work to come. In preparation, the great record-keeping tome must be opened to a fresh blank page. Next, ascending the telescope steps to inspect and clean the instrument, and finally the sun has emerged from the mountain and the great dome doors can be opened; let there be light! With great effort and much precision push and pull of the instruments, the tracking of the sun's progress begins. Now it's time to watch and wait. Clouds and moisture can be an issue and then the dome has to be closed and the daily observation mission aborted. If this were to happen there is always plenty more to do...caring for instrumentation is one of many top priorities, –lubricating moving parts, changing codes, and doing general building maintenance is required too.

Lisa Waters demonstrating magnetic fields and effects on the sun at the local astronomy community event, Astroday in West Hawaii.

All these daily labors of love are done by this sparse crew and they work mostly alone. They welcome the rare occasions when visitors arrive for educational tours and they have the opportunity to share the facility, equipment, and the solar science. On some occasions, when big equipment and/or heavy parts must be managed, then contractors are hired (MLSO installed a new dome in January 2016). As day light fades, the instrumentation is parked and the great doors, if still open, are now closed for the night. Ben returns to the sea by the same lonely road, saluting the sun as it falls below the horizon. It requires a unique and dedicated individual to handle the unusual working conditions at MLSO, an individual that can tolerate the extreme quite of this solitary and remote area, and a person that can accept the constantly changing and extreme weather conditions of a ruggedly high-altitude office location, but our team, the unsung heroes of Mauna Loa, seem to thrive.

Facts and figures:
3.5 hours driving, 10 hours on site.
Ben Berkey (Hilo, HI) and Allen Stueben (Kona, HI) are full time. Lisa Waters is 3/4 time. Greg is a casual.
Work schedule:
Ben works Monday, Wednesday, Friday.
Allen works Tuesday, Thursday, Saturday.
Lisa works as a floater, nominally every other Sunday with 3 other days of overlap with either Allen or Ben during a 2 week period.
Greg works ever other Sunday.

The road to Mauna Loa Observatory.

A note from Ben: The altitude tends to make things take a little longer than normal. People think slower and physical exertion is harder. We have a ~500 foot walk up the hill (~30 foot elevation gain) from the parking lot which often makes me feel a bit out of shape especially if I am jogging. Jogging might be required if some clouds roll in while I am at the restroom down by the parking lot and I need to hustle up to the observatory to close the dome or otherwise react.

Written by Ben Berkey and Wendy Hawkins.

End of an era: The Mauna Loa K-coronameter is decommissioned

kolinski — Thu, 02 Dec 2021 18:11:23 +0000

End of an era: The Mauna Loa K-coronameter is decommissioned kolinski Thu, 12/02/2021 - 11:11

Author:

kolinski

Dec 2, 2021

The Mauna Loa Solar Observatory (MLSO) K-coronameter (Mk4), was decommissioned on August 2, 2013, to be replaced by the new COSMO K-coronagraph.

Mk3 on the MLSO spar

With the approach of the SOlar Heliophysics Observatory (SOHO) Mission, HAO designed and implemented upgrades to the Mk3, known as Mk4, which included the installation of a CCD detector to replace the original diode array, a better polarizing beam splitter, and mechanically stable calibration tilt plate registration. Mk4 has continued to operate until the present. The Mk3/4 K-coronameter has provided 33 years of low coronal observations from the maximum of solar cycle 20 to the maximum of solar cycle 24 acquiring over a half a million images, recording over 1000 CMEs, and observing the brightness and morphological changes of the corona with solar cycle activity.

The Mk3-Koronameter team in Hawaii. L to R: Charlie Garcia, Ed Lundin, Paul Seagraves, Cheryl Baker, Eric Yasukawa, David Sime, Dick Fisher.

HAO Mk3 lead engineer, Bob Lee, setting up the HAO eclipse telescope.

The Mk3 K-coronameter (right) and ancillary equipment are lowered into the Mauna Loa dome in 1979.

The K-coronameter will be replaced by the COSMO K-coronagraph (K-cor), an entirely new instrument which will produce images with 10 times better signal-to-noise and 12 times faster image cadence than the K-coronameter. K-cor will begin providing data in the fall of 2013.

All of the Mk3/Mk4 observations since 1980 are available from HAO’s Mauna Loa homepage

Updates

August 6th: The Mk4 Coronameter has been removed from the MLSO spar! Here is a time-lapse of the operation:

The Mauna Loa Solar Observatory is getting a couple of new instruments in the next year and the first - an instrument to study the large-scale solar corona and launch of coronal mass ejections (CMEs) - is about to be shipped from Boulder to Hawaii. Naturally, we have to take off the old before installing the new so this time-lapse shows the old "ACOS" system (including the Mk 4 Coronagraph) being taken off of the Sun-pointing spar in the observatory dome.

HAO recognizes the many scientists, engineers, observers and support staff who were responsible for the design, fabrication, testing, software, operation, repair, calibration, processing and dissemination of the Mk3/Mk4 instrument and observations:

Richard Fisher, and in reverse alphabetical order: Eric Yasukawa, Oran (Richard) White, Lisa Waters, F. Telang, Allen Stueben, Jack Streete, Kim Streander, Andrew Stanger, Ackley Smith, Leonard Sitongia, David Sime, Rick Sheffer, Paul Seagraves, Paula Rubin, Greg Rose, Steve Rogers, Kristine Rock, Art Poland, Gordon Newkirk, Richard Munro, Greg Muir, C. Muir, Robert MacQueen, Ed Lundin, Ron Lull, Robert Lee, Alice Lecinski, Terry Leach, Loren Laramore, Lee Lacey. Darryl Koon, Don Kolinski, Art Hundhausen, Howard Hull, Tom Holzer, E. Harper, Holly Gilbert, Charlie Garcia, Dennis Gallagher, John Firor, Frank Everts, David Elmore, Giuliana deToma, Tony Darnell, Duc Chu, Clarke Chambellan, Jay Chalmers, Greg Card, Joan Burkepile, Ben Berkey, Cheryl Baker and a host of others including many student assistants.

A New Coronagraph for Mauna Loa

kolinski — Wed, 01 Dec 2021 21:36:31 +0000

A New Coronagraph for Mauna Loa kolinski Wed, 12/01/2021 - 14:36

Author:

kolinski

Dec 1, 2021

NCAR's High Altitude Observatory (HAO) will be installing a new white light coronagraph at the Mauna Loa Solar Observatory (MLSO) in Hawaii in August of this year (2013). A coronagraph is an instrument designed to mimic a total solar eclipse, which occurs when the moon completely occults the solar disk. The new coronagraph, known as K-cor, was designed by HAO engineers and scientists, along with two engineering consultants. K-cor will replace the 1-D scanning coronameter at Mauna Loa known as the Mk4. K-cor will provide a factor of ten improvement in speed and signal-to-noise as well as significant advancements in calibration accuracy and reliability.

It is specially designed to acquire images of the lowest region of the very faint, hot solar atmosphere known as the corona. With a field-of-view of 1.05 to 3.0 solar radii, and a time cadence of 15 seconds, the K-cor will provide unprecedented white light imaging for studying the birth and evolution of coronal mass ejections (CMEs). CMEs are dramatic eruptions in the solar atmosphere that hurl millions of tons of magnetized plasma into the solar wind that can create severe space weather at Earth and throughout the heliosphere. High time cadence images of the low corona provide crucial observations for understanding the formation of CMEs and CME-driven shocks in the solar wind.

A sequence of coronal images from Mk4 showing a CME erupting through the corona in May 2001.

Electrical engineer, Brandon Larson, and Technician Rob Graves install the K-cor center section onto the solar spar at the NCAR Mesa Lab in Boulder.

K-cor has been successfully deployed to the HAO solar spar in Boulder, Colorado. The deployment required careful alignment of the optical systems beginning with the installation of the primary objective lens near the front of the telescope. The objective lens is bombarded by light from the solar surface, which is a million times brighter than the faint corona. The lens must be nearly free of scratches, striations and any blemishes that will cause light to scatter and overwhelm the faint signal coming from the corona.

K-cor occulter

The back end of the K-cor instrument contains the occulter, filters, polarization modulator, lenses and cameras. The system is carefully designed to filter out all unwanted light and capture the all-important polarized light scattered by the electrons in the Sun’s corona. If the corona were not polarized it would not be possible with current technologies to observe it in white light from the ground except during a total solar eclipse. The white object at center left in the image is the K-cor occulter, illuminated by, and blocking, the bright light from the solar surface.

K-cor system testing at the Mesa spar by project manager Scott Sewell and electrical engineer Brandon Larson.

K-cor is undergoing spar testing before it is fully deployed to the Mauna Loa spar in August. The pristine skies at MLSO provide the ideal sky conditions needed to observe the faint corona. HAO engineers and scientists will work with the Mauna Loa observers (Allen Stueben, Ben Berkey, Greg Rose and Lisa Waters) to complete the installation at MLSO by September.

K-cor instrument scientist Alfred de Wijn inspects the calibration optics at the Mesa spar in Boulder.

Following installation at the Mauna Loa spar, K-cor will begin routine observations of the corona. Final checks on data calibration by HAO scientists, led by Alfred deWijn (pictured at left,) will be completed and cross-checked to space-based coronagraph observations to ensure the community receives highest quality dataset. All K-cor observations will be provided via the Mauna Loa website.

K-Cor H-alpha image

An image of the solar corona taken with the K-cor in a neutral emission line of hydrogen known as H-alpha. The dark circle is the projection of the occulter obscuring the solar disk. The two bright features are dense, cool objects known as prominences which may play a key role in the dynamical processes that result in CME formation.

instrumentation

HAO flew observers to MLSO to observe the Sun during the solar eclipse

Recent News

MLSO UCoMP Science Data Now Available

Recent News

A Spectroscopic Survey of Infrared 1–4 μm Spectra in Regions of Prominent Solar Coronal Emission Lines of Fe XIII, Si X, and Si IX

Recent News

NSF Approves Funding for COSMO Next Stage

Recent News

COSMO Site and Design Advancement Updates

Recent NSF Funding for COSMO Site and Design Advancement (COSADA)

Final Design of COSMO Large Coronagraph (LC)

COSMO Site Survey

Recent News

UCoMP Instrument Nearing Science Mission Phase

Recent News

MLSO Facility gets a new dome!

Recent News

Outreach and Observing at Mauna Loa in Hawaii

Recent News

End of an era: The Mauna Loa K-coronameter is decommissioned

Updates

Recent News

A New Coronagraph for Mauna Loa

Recent News