OUR DEEPEST EXPLORATION OF THE UNIVERSE IN X-RAYS

eROSITA is an X-ray space telescope that was launched on July 13, 2019 by an international collaboration, mainly funded by Germany and Russia. The space telescope took its first ever X-ray image three months after orbiting the Earth the following October and has already released some of the first data collected in the first months of operation as well as a schedule confirming the official first data release by December 2022. Most recently, the Astronomy and Astrophysics peer-reviewed science journal has released a special issue including ~35 publications that analyze new eROSITA data. Given the exciting first light and the already big discoveries the telescope has made including the largest supernova remnant ever discovered in X-rays, I thought it would be appropriate to highlight a little bit more about the telescope on my blog! 😄

The eROSITA telescope flies aboard a large satellite: the Spektrum-Röntgen-Gamma (SRG) space satellite. Along with the primary instrument, eROSITA (extended ROentgen Survey with an Imaging Telescope Array), on the SRG is the Russian ART-XC instrument which can probe higher energy X-rays than eROSITA.

As you have probably guessed, this is an X-ray imaging space telescope. It turns out that the Earth’s atmosphere actually absorbs incoming X-rays (see image below).

This is precisely why all astrophysical X-ray instruments are deployed in space including eROSITA.

eROSITA is made up of seven identical and strategically aligned X-ray Mirror Assemblies (MAs) that are situated on an optical bench. Underneath this is the rest of the supporting structure (see the schematic view below), which includes connecting the MAs to the camera assemblies (CAs), i.e. the mirrors will deflect incoming X-rays from its surface in very tiny incident angles that then focus the incoming X-rays onto the cameras (called the grazing incidence angle and is a common practice for designing sensitive X-ray instruments).

The X-ray “baffles” are used to prevent X-ray photons that are outside of the field of view from contaminating the image being taken at that time. This is particularly important when you need to observe an object that may have bright X-ray sources nearby that can contaminate the X-ray measurements.

The telescope (not SRG, the observatory it is deployed on right now) itself is 1.9 meters wide and 3.2 meters high. For my American readers that is about 6 by 10 feet! 😀 The completed instrument weighs in at a whopping 808 kg or 1781 pounds!

The Field Of View (FOV) of the full instrument (including all seven cameras) is about 1 degree in diameter. To give you an idea of what portion of the sky eROSITA can see at any given time, the full moon is about 1/2 a degree in the night sky, so eROSITA is able to see an area in the sky that is 2 times larger than the full moon.

This FOV is considerably larger than both of the previously most sensitive X-ray space telescopes, Chandra and XMM-Newton. Further, eROSITA will operate optimally for a specific energy range of X-ray photons. You will almost always see X-ray astronomy use kiloelectron volts to describe the X-ray energies,

$1 \text{keV} = 1,000 \text{eV} = 1.6 \times 10^{-12} \text{Joules}$

eROSITA, along with Chandra, XMM-Newton, and several other currently operating (and retired) X-ray instruments, can detect X-ray photons between 0.2 keV and 10 keV (see image below, but don’t freak out 😉)

The above plot is showing the field of view averaged effective area in cm squared as a function of energy. You can think of this as the sensitivity of the instrument as a function of energy. Each line corresponds to a different instrument: eROSITA’s seven modules in solid red, Chandra’s ACIS-I setup in green dot-dashed, another Chandra instrument called HRC-I in purple dashed, XMM-Newton’s 3 cameras with the thin filter on, and the previously retired ROSAT PSCPC instrument.

You can see that eROSITA is just about the most sensitive instrument from energies ~0.5keV to ~2keV which is often referred to as the soft X-ray range which just indicates the lower energy range of the X-ray band. Above 2 keV, the sensitivity of eROSITA drops off at a similar rate as the Chandra instruments, while XMM-Newton wins the sensitivity competition at energies greater than about 2keV. With its large field of view in comparison to Chandra and XMM-Newton, eROSITA will make (and has already demonstrated) significant discoveries to X-ray astronomy.

What separates eROSITA from other current missions like Chandra, in addition to its large field of view and sensitivity, is its angular and energy resolution and most of all — the way it will take data. Chandra and XMM-Newton X-ray telescopes are pointing missions. This means the telescope has to position itself for specific observations in varying parts of the sky. The time gets “shared” among thousands of researchers who request for telescope observations every year. eROSITA, on the other hand, is an all-sky survey.

It is the first ever X-ray instrument to survey the entire sky from 0.2-10keV in astronomy HISTORY!

ROSAT was also an all-sky survey, but it only imaged soft X-ray photons, so it didn’t detect X-ray photons with energy more than 2.4keV. ROSAT also had a similar field of view of 2 degrees, but by inspecting the above effective area (i.e. sensitivity) plot, we can see that eROSITA will be a much deeper sky survey, by about 4 times!

To visualize this difference, here is a ROSAT view of the Vela supernova remnant (if you are familiar with my work you have seen the ROSAT image before) in the left panel below compared to the Vela SNR image from eROSITA on the right. I’m unable to find more details about the eROSITA image, but I’m guessing that the colors indicate three energy bands: red is likely the softest of X-rays < 0.6 keV, green is probably “medium” X-rays from 0.6 – 1-ish keV, and blue is likely 1-2.3 keV energies. If this assumption is correct, most of the Vela SNR is dominated by soft and medium X-rays (which is indeed the case, see the ROSAT image on the left lol!). We can also see the smaller overlapping supernova remnant Puppis A is bright in this X-ray range in both images, but that “hard” (higher-energy, see eROSITA image) X-rays dominate the observed emission. Additionally, one can easily spot the Vela central pulsar (lots of hard X-rays there in blue, too!) in the near-center of the eROSITA image, and a third supernova remnant in the lower left corner, visible by only a faint circular blue hue. Neither the central pulsar nor the lower-left supernova remnant is resolved in the ROSAT image. Note: do I see the third supernova remnant’s central compact object in the eROSITA image?!

First light for theeROSITA telescope occurred in mid-October just months after launch

Moreover, eROSITA has already detected 10 times more sources than ROSAT which is about as many as have been discovered by all previous X-ray missions combined. Less than a year after launch, eROSITA has already completed its first all-sky survey, one of eight anticipated full sky surveys.

eROSITA’s first all-sky survey will be released in 2022 (well, the half that the Germans own), reporting already thousands of new sources, most being active galactic nuclei. One of the exciting discoveries includes the largest supernova remnant discovered in X-rays to date which has been nicknamed “Hoinga”. There are a lot of special surprises associated with Hoinga, including its high location with respect to the Galactic plane, an unusual location for supernova remnants to be found.

Hoinga is estimated to have a diameter of about 4.4 degrees. Vela SNR has a diameter of 8 degrees, but it was discovered first in radio, not X-ray.

To conclude, here is a super cool visual graphic about the SRG observatory where eROSITA operates.

I will definitely be on the lookout 👀 for the first data release, although that means I will have to learn (yet another) new software to clean and analyze the data….. 🥵 😅

A random side note

What I think is extra intriguing about this telescope is the collaboration between Germany and Russia (Just hear me out lol). The terms of the collaboration seem a little unusual. They have defined a German half of the X-ray sky as well as a Russia half of the X-ray sky. Essentially the Western hemisphere of the Galaxy (in Galactic coordinates) is owned by the Germans with unique scientific data exploitation rights and the Eastern hemisphere belongs to the Russians. They have decided to equally share the all-sky surveys, so I suppose the data that has been divided will include individual mission projects i.e. pointed observations for a particular object will have certain proprietary rights depending on its location in the sky. With that being said, only the German half of the sky has been scheduled a public release of data for 2022, and all of the Russian X-ray data and its release schedule is to be determined.

It will be very interesting to see how the data-sharing pans out with this particular method. To be fair, I’m not totally sure if this is a standard practice in international space efforts such as this, but I would be surprised if it is.

YEAR TWO AT CLEMSON

My second year at Clemson was just as difficult and overwhelming as the first year (yay). Because I was “year-zero” (see this post for more) my first year, I was required to take one year of lower-level (undergraduate) physics courses before enrolling in the official graduate-level courses. So, “year one” really began my second year when I enrolled into the graduate level courses of the physics program: Classical Mechanics (I), Quantum Mechanics (I&II), Mathematical Methods, Statistical Mechanics, and Electromagnetism. I’d like to say that the prior year of taking very similar courses that I breezed through my year one, but that would be a big fat lie 😅. I struggled the whole way through. When I say I was studying morning and night and most of my weekends, I mean that. A small group of us in class would regularly work together on homework problems and study for tests. We continued to do this the entire year and even into the summer following the end of year one, when we were all required to prepare and take the Written Qualification Examinations (ooooooeeeeooooooo 👻🙀)

There are three “quals” that all PhD students HAVE to pass if they want to continue their PhD research at Clemson: Classical & Statistical Mechanics were on one exam, Quantum Mechanics on the second, and Electromagnetic Theory on the third. Every student is required to pass all three.

Like, can you JUST IMAGINE THE STRESS WE ARE UNDER?!?!!?!? CAN YOU?!?!?!

The three quals are given each their own examination day with up to four hours to work on 6-8 problems over the course of one week. And if that’s not horrifying enough, the entire department then confers together and discuss/debate/challenge students’ performances on the tests. I am certain I speak for the entire graduate student body in the Clemson Physics PhD program, but this was my own personal hell. I still torture myself wondering what was said in that conference room about my performance 😩.

There is a light at the end of the tunnel though!

The first 1-2 years are very clearly a stressful time of the early PhD career as a Clemson graduate student, but it really is a whole lot different after you finally make it past the Written Qual bump! At this point, you are done with your core coursework and can now finally start earning some research credits and start focusing on the stuff that you came here for.

This moment comes at the end of the year one – once you have finished those six graduate courses; you’ve taken all the final exams and have all your final grades, which is generally a time to rejoice and relax, right?

The clock actually just started. And it’s ticking. You got three (3!!) months to prepare for possibly the most difficult obstacle of your academic career. To be fair, you did also have about 1-2 years of relevant coursework that will hopefully come in handy.

Are you guys sweating just reading this?

Cause I actually have another complication to throw into the mix. This one is a given though, and hopefully doesn’t catch anyone by surprise, since it is a common practice for both undergraduate and graduate students. This concept is the measure of academic standing, aka needing to meet a minimum grade requirement to continue as a student in the program. This part can be confusing as a fresh graduate student, because you come into the program and you start hearing about how “GPAs don’t matter at this point” and how it’s really your research background and skillset. I am not really sure where exactly that should apply because even now as I prepare for postdoctoral positions after graduation, they all ask for transcripts with complete grades lol.

P.S. University: could it maybe not cost me \$15 to send my own academic record (electronic, too; what does that cost you to send an e-mail, I mean really) to potential employers?!

Idk, maybe they are just trying to make you feel better because it can be hard for some students who come into the program and are used to being the top of their class, but then they are making 50% on tests (which can sometimes be a class average) and they will beat themselves up over it even if it’s the highest grade in the class (not kidding, I’ve seen it!).

The bottom line is, you actually do have to have a minimum GPA of 3.0 to remain in good academic standing with the graduate school. So, your GPA does actually matter even in graduate school. At the very least, it matters the most those first 1-2 years when you are actually taking coursework. This can be tricky to maneuver your first year and is even harder if you don’t have the right support or guidance.

I wish I could offer up some advice for this delicate time in your PhD, but I don’t really have anything general enough to share here. We are all going to have different education levels coming into the program. Some students are coming in with two degrees in Physics already and others just completed their 4-year degree in Chemistry. The resources you require to get past the written quals will vary because of this. The written placement test you take when you first arrive at Clemson is meant to help you anticipate where you may fall among your incoming class. You will also have an opportunity to discuss your placement test score with the graduate student coordinator (GRC) who should ideally provide you with the most likely path for you to succeed.

Gosh. My post about my second year turned into the cliff notes version of the graduate student handbook. My b y’all. That whole year is honestly pretty blurry for me (and uneventful, as you may have guessed). The one thing that sticks out to me that year was meeting Noah ❣️ (my beau). We were neighbors and met at the community pool at our apartment complex the summer before heading into those graduate courses. Oh, I also got my first cat on September 11, 2017 — during the fall semester of year one. It was when a tropical storm swept through the Southeast and cut the power to much of the area for about 24 hours. Naturally me, my boyfriend, and my roommate decided to go to PetSmart to get a toy for Ruca (yes, during a tropical storm 🧐) and came home with my cat, Mars. No, Mars was not the toy. He is 4.5 years old now and has established my morning routine for me.

Below I share the social media post featuring me and one of my best study buddies from year one when we learned that we passed our written quals! Allen and I spent (what felt like) every waking moment together studying for those exams. I miss arguing with you, Allen! Cheers to good memories but many more cheers to having this stressful time of our lives far away in the past 🤓.

WARNING: the caption text features a couple expletives, I do apologize.

Please note the aformentioned PhD requirements are specific to Clemson’s physics PhD program. Each program varies even just among the graduate school at Clemson and at each academic institution.